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The Hamburg/RASS Catalogue of optical identifications. Northern high-galactic latitude ROSAT Bright Source Catalogue X-ray sources
We present the Hamburg/RASS Catalogue (HRC) of optical identificationsof X-ray sources at high-galactic latitude. The HRC includes all X-raysources from the ROSAT Bright Source Catalogue (RASS-BSC) with galacticlatitude |b| >=30degr and declination delta >=0degr . In thispart of the sky covering ~ 10 000 deg2 the RASS-BSC contains5341 X-ray sources. For the optical identification we used blue Schmidtprism and direct plates taken for the northern hemisphere Hamburg QuasarSurvey (HQS) which are now available in digitized form. The limitingmagnitudes are 18.5 and 20, respectively. For 82% of the selectedRASS-BSC an identification could be given. For the rest either nocounterpart was visible in the error circle or a plausibleidentification was not possible. With ~ 42% AGN represent the largestgroup of X-ray emitters, ~ 31% have a stellar counterpart, whereasgalaxies and cluster of galaxies comprise only ~ 4% and ~ 5%,respectively. In ~ 3% of the RASS-BSC sources no object was visible onour blue direct plates within 40\arcsec around the X-ray sourceposition. The catalogue is used as a source for the selection of(nearly) complete samples of the various classes of X-ray emitters.
| EUV activity in late-type stars during the ROSAT WFC All-Sky Survey - I. Techniques and initial results
We study 127 active late-type stars, including the well-known flarestars, in the extreme ultraviolet (EUV) region of the electromagneticspectrum, using the ROSAT Wide Field Camera (WFC) survey observations.Our analysis includes photometry for all the stars in the sample, timinganalysis of the observed photon events, and a statistical analysis forpossible small-scale, low-level variability. 49 stars in our sample weredetected in one or both EUV wavebands. A total of 35 flares were seen,from 23 stars, not all of them well-known flare stars. In addition,about half of the detections exhibited low-level variability. Furtheranalysis reveals that the observed low-level variability was not due torotational or orbital modulation, but rather was related to small-scaleactivity on the stars, possibly in the form of small-amplitude,flare-like events which were too faint to be recognized as individualflares at the sensitivity of the WFC. We call this low-level activity`milliflaring'. We also give estimated upper-limit count rates for thenon-detections.
| HIPPARCOS distances of X-ray selected stars: implications on their nature as stellar population.
We present the parallaxes, measured by Hipparcos, for a sample of X-rayselected stars. The stars belong to the stellar sample of the EinsteinExtended Medium Sensitivity Survey. They are all at galactic latitude|b|>20deg, and are generally far away from known star formingregions. Several of these stars show lithium abundance and activitylevel typical of very young stars with ages comparable to that of thePleiades. We show that the majority of our sample stars are on the mainsequence, with only =~20% being giants. We do not find a significantpresence of pre-main sequence stars in our sample, notwithstanding thefact that some of our stars have a considerable lithium abundance,showing that the stars observed are most likely young and activemain-sequence objects.
| Activity in X-ray-selected late-type stars
A spectroscopic study has been conducted of nine X-ray bright late-typestars selected from two Einstein X-ray surveys: the ColumbiaAstrophysical Laboratory Survey (five stars) and the CFA MediumSensitivity Survey (MSS; four stars). Spectral classes were determinedand radial and V sin(i) velocities were measured for the stars. Four ofthe Columbia Survey stars were found to be new RS CVn-type binaries. Thefifth Columbia survey star was found to be an active G dwarf starwithout evidence for binarity. None of the four MSS stars were found tobe either binaries or optically active stars. Activity in these starswas assessed by measuring the excess emission in H-alpha and the Ca IIIRT (8498, 8542) lines in comparison with inactive stars of similarspectral types. A correlation was found between X-ray luminosity and Vsin(i) and H-alpha line excess. The measured excess line emission inH-alpha was also correlated with V sin(i) but not with the IRT lineexcess.
| The Einstein Observatory Medium Sensitivity Survey - Optical identifications for a complete sample of X-ray sources
It is suggested that virtually all the X-ray sources in the EinsteinObservatory's Medium Sensitivity Survey flux range can be identifiedwith objects visible on the POSS, on the basis of the completeidentification of all sources north of -25 deg declination. There is noevidence for a significant population of 'blank field' X-ray sources atthis flux level, and therefore no evidence for any new X-ray sourceclass with very high L(x)/L(v). Most of the quasars detected in thepresent survey are spectroscopically similar to optical orradio-selected quasars. About 25 percent of the quasar sample, however,had reddish colors, and permitted lines dominated by a narrow-linecomponent. These objects form a second sequence of active galacticnuclei, distinct in their optical properties from the broad lineobjects.
| Results from an extensive Einstein stellar survey
The preliminary results of the Einstein Observatory stellar X-ray surveyare presented. To date, 143 soft X-ray sources have been identified withstellar counterparts, leaving no doubt that stars in general constitutea pervasive class of low-luminosity galactic X-ray sources. Stars alongthe entire main sequence, of all luminosity classes, pre-main sequencestars as well as very evolved stars have been detected. Early type OBstars have X-ray luminosities in the range 10 to the 31st to 10 to the34th ergs/s; late type stars show a somewhat lower range of X-rayemission levels, from 10 to the 26th to 10 to the 31st ergs/s. Late typemain-sequence stars show little dependence of X-ray emission levels uponstellar effective temperature; similarly, the observations suggest weak,if any, dependence of X-ray luminosity upon effective gravity. Instead,the data show a broad range of emission levels (about three orders ofmagnitude) throughout the main sequence later than F0.
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| Takýmyýldýz: | Yilan |
| Sað Açýklýk: | 15h35m21.01s |
| Yükselim: | +09°08'06.5" |
| Görünürdeki Parlaklýk: | 8.138 |
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