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The ROSAT All-Sky Survey Catalogue of the Nearby Stars?

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The ROSAT All-Sky Survey Catalogue of the Nearby Stars? ASTRONOMY & ASTROPHYSICS MARCH I 1999, PAGE 319 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 135, 319–338 (1999) The ROSAT all-sky survey catalogue of the nearby stars? M. H¨unsch1, J.H.M.M. Schmitt2,4, M.F. Sterzik3,4, and W. Voges4 1 Institut f¨ur Theoretische Physik und Astrophysik, Universit¨at Kiel, Olshausenstrasse 40, 24118 Kiel, Germany 2 Hamburger Sternwarte, Universit¨at Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany 3 European Southern Observatory, Casilla 19001, Santiago 19, Chile 4 Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstr. 1, 85740 Garching, Germany Received October 16, accepted November 16, 1998 Abstract. We present X-ray data for all entries of the cf. Haisch & Schmitt 1996; Acton 1996) during the solar Third Catalogue of Nearby Stars (Gliese & Jahreiß 1991) cycle and is known to be strongly correlated with other that have been detected as X-ray sources in the ROSAT magnetic activity indicators (e.g., sunspot numbers, flare all-sky survey. The catalogue contains 1252 entries yield- frequency, chromospheric Ca ii emission). Hence, X-ray ing an average detection rate of 32.9 percent. In addi- luminosity can be regarded as a good activity indicator tion to count rates, source detection parameters, hardness also for other late-type stars. Conversely, X-ray emission ratios, and X-ray fluxes we also list X-ray luminosities from O- and early B-type stars obeys (approximately) a −7 derived from Hipparcos parallaxes. Lx/Lbol ≈ 10 relation and is attributed to shocks gen- erated and dissipated within the radiatively driven winds Key words: stars: activity — stars: coronae — stars: of those stars. late-type — X-rays: stars A thorough investigation of the properties of stellar X-ray emission requires large samples of stars in order to reduce the effects of individual scatter and to con- struct samples of stars with given properties such as mass, age, rotation rate etc. Especially important are complete, 1. Introduction volume-limited samples of stars, for example, to derive X-ray luminosity distribution functions. In principle, there One of the major results obtained with the imaging X-ray are two different approaches: i) to construct such a telescopes flown onboard the Einstein and ROSAT ob- complete sample and to look for X-ray emission from servatories is the ubiquity of X-ray emission from normal those stars afterwards, and ii) to scan the whole sky for stars throughout the whole Hertzsprung-Russell (HR) di- X-ray emission and then to extract the data for the sample agram, the only exceptions being A-type main sequence stars (input positions). The first method has been applied stars and some of the late-type giants and supergiants. by Schmitt et al. (1995) and Schmitt (1997) for the im- However, the more sensitive ROSAT observations have re- mediate solar environment, i.e., the K- and M-type stars vealed X-ray emission even from those types of stars. within 7 pc and the A-, F-, and G-type stars within 13 pc X-ray emission from late-type stars is generally at- from the Sun, respectively. These investigations revealed tributed to magnetically heated stellar coronae. As that virtually every late-type dwarf star with spectral suggested by the example of the Sun’s corona, the type later than A7 can be detected as an X-ray source 6 X-ray emitting hot (> 10 K) plasma is believed to be given data of sufficient sensitivity. These data are from confined by coronal magnetic fields, which ultimately both the ROSAT all-sky survey (RASS) and deep individ- originate from the interaction between rotation and ual pointed ROSAT observations. A similar investigation outer convection zones. The solar X-ray luminosity on late-type giants within 25 pc has been performed by 25 27 −1 varies approximately between 3 10 and 1 10 erg s H¨unsch et al. (1996). ˚ (extrapolated to a 1 − 300 A “bolometric X-ray band”; The second method requires the existence of a suffi- Send offprint requests to:M.H¨unsch, ciently deep all-sky survey. Until now, the ROSAT ob- e-mail: [email protected] servatory has undertaken the only sensitive X-ray sur- ? Catalogue also available at CDS via anonymous ftp vey. These data provide a flux-limited but otherwise un- to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u- biased sample of X-ray sources (Voges et al. 1996a). Of strasbg.fr/Abstract.html the ≈ 1.5105 detected sources, about one third are 320 M. H¨unsch et al.: The ROSAT all-sky survey catalogue of the nearby stars considered to be coronal. We used these data to search given a typical energy-conversion factor for soft sources for X-ray emission from stars contained in the Catalogue of 6 10−12 erg cts−1 cm−2 (cf. Sect. 2.3) the typical de- of Nearby stars (the so-called Gliese catalogue; Gliese & tection limit of RASS observations amounts to a limiting −13 −2 −1 Jahreiß 1991). The Gliese catalogue is the most compre- flux of fx ≈ 10 erg cm s . At the distance limit of hensive list of stars in the solar environment and it is the Gliese catalogue, i.e., at 25 pc, this corresponds to an 27 −1 proposed to be as complete as possible within a space vol- X-ray luminosity of Lx ≈ 7.510 erg s . Note that this is ume of 25 pc radius around the Sun. Our investigation is not an average value for the detection limit for the Gliese limited in completeness by both the completeness of the stars since many stars are closer and the exposure time Gliese catalogue and the sensitivity of the RASS. However, increases towards the ecliptic poles. also for those Gliese stars that are not detected, it is in For a more detailed description of the RASS we refer principle possible to estimate upper limits for their X-ray to Voges (1992) and Belloni et al. (1994). Details of the luminosity (see Sect. 2.1). ROSAT observatory in general can be found in Tr¨umper A preliminary investigation of stellar activity of the (1983) and Tr¨umper et al. (1991). The PSPC detector nearby stars based on the data presented here has already used during the RASS is described by Pfeffermann et al. been performed by Sterzik & Schmitt (1997). However, (1986). In February 1997 the remaining gaps left in the all- X-ray luminosities for those stars derived from ROSAT sky survey were filled with a sequence of more than 500 data combined with Hipparcos parallaxes are presented pointed, partially overlapping PSPC observations so that here for the first time. with the exception of a small region around the strong We have also performed similar surveys of X-ray emis- X-ray source Sco X-1 the whole sky has been imaged with sion from the stars contained in the Bright Star catalogue the ROSAT PSPC. In the catalogue presented in this pa- (BSC; Hoffleit & Warren 1991). These results are pre- per we include sources detected in this “survey repair” sented as catalogues of X-ray data, which have already pointed observations; they are marked with an asterisk. been published for OB stars (Bergh¨ofer et al. 1996), late- The source detection was performed by means of a type giants and supergiants (H¨unsch et al. 1998a; hereafter maximum likelihood algorithm (Cruddace et al. 1988) in HSV98), and late-type main-sequence stars and subgiant the course of the standard analysis software system (SASS; stars (H¨unsch et al. 1998b). Voges et al. 1992). The significance of an X-ray source is expressed by the likelihood Li = –ln(1–P ), where P is the probability of existence; e.g., a likelihood of Li = 7 2. RASS data and detection of late-type stars corresponds to a source existence probability of 99.9%. The result of the SASS is a comprehensive list of approx- 2.1. The ROSAT all-sky survey (RASS) imately 105 sources, each described by the sky position in right ascension and declination, its source detection likeli- During its first half year of operations, the ROSAT obser- hood, count rate, hardness ratios, extent, and correspond- vatory carried out the first all-sky survey with an imag- ing errors. The data for the brighter X-ray sources have ing X-ray telescope between July 1990 and January 1991. been released as the ROSAT All-sky Survey Bright Source Further survey observations were carried out in February Catalogue (Voges et al. 1996b), which contains sources 1991 (2 days) and August 1991 (10 days). The whole sky with Likelihood ≥ 15, count rate larger than 0.05 s−1, was scanned along great circles perpendicular to the di- and with at least 15 detected photons. rection to the Sun. Because of the Earth’s motion around the Sun, the plane of these circles slowly (1◦/d) rotated around an axis through the ecliptic poles, thus covering 2.2. Identification of X-ray sources with nearby stars the whole celestial sphere within 6 months. Each point of the sky was observed several times as the scan paths of 2 We used the Third Catalogue of Nearby Stars (Gliese degrees width (i.e., the field of view of the PSPC detec- & Jahreiß 1991) as input sample for our search of tor) progressed along the ecliptic. Therefore, the data of X-ray bright nearby stars. That input sample consists of any particular source consist of a number of “snapshots” 3802 stars. of up to 30 s duration, separated by the orbital period of The procedure whereby the positions of RASS sources the satellite (≈ 90 min) and distributed over an interval were matched with the stars of our input sample is the of at least 2 days.
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