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Search for associations containing young stars (SACY). I. Sample and searching method
We report results from a high-resolution optical spectroscopic surveyaimed to search for nearby young associations and young stars amongoptical counterparts of ROSAT All-Sky Survey X-ray sources in theSouthern Hemisphere. We selected 1953 late-type (B-V~≥~0.6),potentially young, optical counterparts out of a total of 9574 1RXSsources for follow-up observations. At least one high-resolutionspectrum was obtained for each of 1511 targets. This paper is the firstin a series presenting the results of the SACY survey. Here we describeour sample and our observations. We describe a convergence method in the(UVW) velocity space to find associations. As an example, we discuss thevalidity of this method in the framework of the β Pic Association.
| X-ray flare in XRF 050406: evidence for prolonged engine activity
We present observations of XRF 050406, the firstburst detected by Swift showing a flare in its X-ray light curve. Duringthis flare, which peaks at t_peak ˜ 210 s after the BAT trigger, aflux variation of ? F / F ˜ 6 in a very short time ? t/ t_peak ? 1 was observed. Its measured fluence in the 0.2-10 keVband was ~1.4 × 10-8 erg cm-2, whichcorresponds to 1-15% of the prompt fluence. We present indications ofspectral variations during the flare. We argue that the producingmechanism is late internal shocks, which implies that the central engineis still active at 210 s, though with a reduced power with respect tothe prompt emission. The X-ray light curve flattens to a very shallowslope with decay index of ~0.5 after ~4400 s, which also supportscontinued central engine activity at late times. This burst isclassified as an X-ray flash, with a relatively low fluence(~10-7 erg cm-2 in the 15-350 keV band, E_iso˜ 1051 erg), a soft spectrum (photon index 2.65), nosignificant flux above ~50 keV and a peak energy Ep < 15keV. XRF 050406 is one of the first examples of a well-studied X-raylight curve of an XRF. We show that the main afterglow characteristicsare qualitatively similar to those of normal GRBs. In particular, X-rayflares superimposed on a power-law light curve have now been seen inboth XRFs and GRBs. This indicates that a similar mechanism may be atwork for both kinds of events.
| The ASCA Medium Sensitivity Survey (the GIS Catalog Project): Source Catalog
We present the first X-ray source catalog of the ASCA Medium SensitivitySurvey (AMSS, or the GIS catalog project), constructed from data atGalactic latitudes b>10deg observed between 1993 May and 1996December. The catalog utilizes 368 combined fields and contains 1343sources with the detection significance above 5 σ either in thesurvey bands of 0.7-7 keV, 2-10 keV, or 0.7-2 keV, including targetsources. For each source, the ASCA source name, position, a 90% errorradius, count rates in the three bands, detection significances, fluxes,and a hardness ratio are provided. With extensive simulations, wecarefully evaluate the data quality of the catalog. Results fromcross-correlation with other existing catalogs are briefly summarized.
| A New Association of Post-T Tauri Stars near the Sun
Observing ROSAT sources in an area 20°×25° centered at thehigh-latitude (b=-59°) active star ER Eri, we found evidences for anearby association, that we call the Horologium association (HorA),formed by at least 10 very young stars, some of them being bona fidepost-T Tauri stars. We suggest other six stars as possible members ofthis proposed association. We examine several requirements thatcharacterize a young stellar association. Although no one of them,isolated, gives an undisputed prove of the existence of the HorA, alltogether practically create a strong evidence for it. In fact, the Liline intensities are between those of the older classical T Tauri starsand the ones of the Local Association stars. The space velocitycomponents of the HorA relative to the Sun (U=-9.5+/-1.0, V=-20.9+/-1.1,W=-2.1+/-1.9) are not far from those of the Local Association, so thatit could be one of its last episodes of star formation. In this regionof the sky there are some hotter and non-X-ray active stars, withsimilar space velocities, that could be the massive members of the HorA,among them, the nearby Be star Achernar. The maximum of the massdistribution function of its probable members is around 0.7-0.9Msolar. We estimate its distance as ~60 pc and its size as~50 pc. If spherical, this size would be larger than the surveyed area,and many other members could have been missed. ER Eri itself was foundto be not a member, but a background RS CVn-like system. We alsoobserved three control regions, two at northern and southern Galacticlatitudes and a third one in the known TW Hya association (TWA), and theproperties and distribution of their young stars strengthen the realityof the HorA. Contrary to the TWA, the only known binaries in the HorAare two very wide systems. The HorA is much more isolated from cloudsand older (~30 Myr) than the TWA and could give some clues about thelifetime of the disks around T Tauri stars. Actually, none of theproposed members is an IRAS source indicating an advanced stage of theevolution of their primitive accreting disks. Based on observations madeunder the Observatório Nacional-ESO agreement for the jointoperation of the 1.52 m ESO telescope and at the Observatório doPico dos Dias, operated by MCT/Laboratório Nacional deAstrofísica, Brazil
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| Takýmyýldýz: | Irmak |
| Sað Açýklýk: | 02h17m43.52s |
| Yükselim: | -50°14'42.3" |
| Görünürdeki Parlaklýk: | 9.248 |
| özdevim Sað Açýklýk: | -3.2 |
| özdevim Yükselim: | 4.4 |
| B-T magnitude: | 10.176 |
| V-T magnitude: | 9.325 |
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