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Mapping the Shores of the Brown Dwarf Desert. III. Young Moving Groups
We present the results of an aperture-masking interferometry survey forsubstellar companions around 67 members of the young (~8-200 Myr) nearby(~5-86 pc) AB Doradus, ? Pictoris, Hercules-Lyra, TW Hya, andTucana-Horologium stellar associations. Observations were made atnear-infrared wavelengths between 1.2 and 3.8 ?m using the adaptiveoptics facilities of the Keck II, Very Large Telescope UT4, and PalomarHale Telescopes. Typical contrast ratios of ~100-200 were achieved atangular separations between ~40 and 320 mas, with our survey being 100%complete for companions with masses below ~0.25 M &sun;across this range. We report the discovery of a 0.52 ± 0.09 M&sun; companion to HIP 14807, as well as the detections andorbits of previously known stellar companions to HD 16760, HD 113449,and HD 160934. We show that the companion to HD 16760 is in a face-onorbit, resulting in an upward revision of its mass from M2sin i ~ 14 M J to M 2 = 0.28 ±0.04 M &sun;. No substellar companions were detected aroundany of our sample members, despite our ability to detect companions withmasses below 80 M J for 50 of our targets: of these, oursensitivity extended down to 40 M J around 30 targets, with asubset of 22 subject to the still more stringent limit of 20 MJ. A statistical analysis of our non-detection of substellarcompanions allows us to place constraints on their frequency around~0.2-1.5 M &sun; stars. In particular, consideringcompanion mass distributions that have been proposed in the literature,we obtain an upper limit estimate of ~9%-11% for the frequency of 20-80M J companions between 3 and 30 AU at 95% confidence,assuming that their semimajor axes are distributed according to d {N}/da\propto a^{-1} in this range.
| RACE-OC project: rotation and variability in the ? Chamaeleontis, Octans, and Argus stellar associations
Context. Rotational properties of late-type low-mass members ofassociations of known age provide a fundamental source of information onstellar internal structure and its evolution. Aims: We aim atdetermining the rotational and magnetic-related activity properties ofstars at different stages of evolution. We focus our attention primarilyon members of young stellar associations of known ages. Specifically, weextend our previous analysis in Paper I (Messina et al. 2010, A&A520, A15) to 3 additional young stellar associations beyond 100 pc andwith ages in the range 6-40 Myr: ? Chamaeleontis (~6 Myr),Octans (~20 Myr), and Argus (~40 Myr). Additional rotational data of? Chamaeleontis and IC 2391 clusters are also considered. Methods: Rotational periods were determined by applying the Lomb-Scargleperiodogram technique to photometric time-series data obtained by theAll Sky Automated Survey (ASAS) and the Wide Angle Search for Planets(SuperWASP) archives. The magnetic activity level was derived from theamplitude of the V light curves. Results: We detected therotational modulation and measured the rotation periods of 56 stars forthe first time, confirmed 11 and revised 3 rotation periods alreadyknown from the literature. Adding the periods of 10 additional starsretrieved from the literature we determined a sample of 80 periodicstars at ages of ~6, ~20, and ~40 Myr. Using the SuperWASP data we alsorevisited some of the targets studied in Paper I. Conclusions:With the present study we have completed the analysis of the rotationalproperties of the late-type members of all known young looseassociations in the solar neighbourhood. Considering also the results ofPaper I, we have derived the rotation periods of 241 targets: 171confirmed, 44 likely, 26 uncertain. The period of the remaining 50 starsknown to be part of loose associations still remains unknown. Therotation period distributions we provided in the 0.8-1.2M&sun; mass range span nine different ages from 1 to ~100Myr. This rotation period catalogue, and specifically the newinformation presented in this paper at ~6, 20, and 40 Myr, contributessignificantly to a better observational description of the angularmomentum evolution of young stars. The results of the angular momentumevolution model based on this period database will be presented inforthcoming papers.Based on the All Sky Automated Survey (ASAS) and Wide Angle Search forPlanets (SuperWASP) photometric data.Appendices A and B are available inelectronic form at http://www.aanda.org
| RACE-OC project: Rotation and variability of young stellar associations within 100 pc
Context. Examining the angular momentum of stars and its interplay withtheir magnetic fields represent a promising way to probe the stellarinternal structure and evolution of low-mass stars. Aims: Weattempt to determine the rotational and magnetic-related activityproperties of stars at different stages of evolution.We focused ourattention primarily on members of clusters and young stellarassociations of known ages. In this study, our targets are 6 young loosestellar associations within 100 pc and with ages in the range 8-70 Myr:TW Hydrae (~8 Myr), ? Pictoris (~10 Myr), Tucana/Horologium,Columba, Carina (~30 Myr), and AB Doradus (~70 Myr). Additionalrotational data for ? Persei and the Pleiades from the literatureare also considered. Methods: Rotational periods of starsexhibiting rotational modulation due to photospheric magnetic activity(i.e., starspots) were determined by applying the Lomb-Scargleperiodogram technique to photometric time-series data obtained by theAll Sky Automated Survey (ASAS). The magnetic activity level was derivedfrom the amplitude of the V lightcurves. The statistical significance ofthe rotational evolution at different ages was inferred by applying atwo-sided Kolmogorov-Smirnov test to subsequent age-bins. Results: We detected the rotational modulation and measured the rotationperiods of 93 stars for the first time, and confirmed the periods of 41stars already known from the literature. For an additional 10 stars, werevised the period determinations by other authors. The sample wasaugmented with periods of 21 additional stars retrieved from theliterature. In this way, for the first time we were able to determinethe largest set of rotation periods at ages of ~8, ~10 and ~30 Myr, aswell as increase by 150% the number of known periodic members of AB Dor. Conclusions: The analysis of the rotation periods in youngstellar associations, supplemented by Orion Nebula Cluster (ONC) and NGC2264 data from the literature, has allowed us to find that in the0.6-1.2 M? range the most significant variations in therotation period distribution are the spin-up between 9 and 30 Myr andthe spin-down between 70 and 110 Myr. Variations of between 30 and 70Myr are rather doubtful, despite the median period indicating asignificant spin-up. The photospheric activity level is found to becorrelated with rotation at ages greater than ~70 Myr and to show someadditional age dependence besides that related to rotation and mass.Tables 1.1-1.7 and Figs. 1.1-1.22 are only available in electronic format http://www.aanda.orgBased on theAll Sky Automated Survey photometric data.
| Search for associations containing young stars (SACY). III. Ages and Li abundances
Context: Our study is a follow-up of the SACY project, an extended highspectral resolution survey of more than two thousand opticalcounterparts to X-ray sources in the southern hemisphere targeted tosearch for young nearby association. Nine associations have either beennewly identified, or have had their member list revised. Groupsbelonging to the Sco-Cen-Oph complex are not considered in the presentstudy. Aims: These nine associations, with ages of between about 6Myr and 70 Myr, form an excellent sample to study the Li depletion inthe pre-main sequence (PMS) evolution. In the present paper, weinvestigate the use of Li abundances as an independent clock toconstrain the PMS evolution. Methods: Using our measurements ofthe equivalent widths of the Li resonance line and assuming fixedmetallicities and microturbulence, we calculated the LTE Li abundancesfor 376 members of various young associations. In addition, weconsidered the effects of their projected stellar rotation.Results: We present the Li depletion as a function of age in the firsthundred million years for the first time for the most extended sample ofLi abundances in young stellar associations. Conclusions: A clearLi depletion can be measured in the temperature range from 5000 K to3500 K for the age span covered by the nine associations studied in thispaper. The age sequence based on the Li-clock agrees well with theisochronal ages, the ?Cha association being the only possibleexception. The lithium depletion patterns for the associations presentedhere resemble those of the young open clusters with similar ages,strengthening the notion that the members proposed for these loose youngassociations have indeed a common physical origin. The observed scatterin the Li abundances hampers the use of Li in determining reliable agesfor individual stars. For velocities above 20 km s-1,rotation seems to play an important role in inhibiting the Li depletion.Based on observations collected at the ESO - La Silla and at theLNA-OPD.Tables [see full textsee full text]-[see full textsee full text] areonly available in electronic form at http://www.aanda.org
| The SOPHIE search for northern extrasolar planets . I. A companion around HD 16760 with mass close to the planet/brown-dwarf transition
We report on the discovery of a substellar companion or a massiveJupiter orbiting the G5V star HD 16760 using the spectrograph SOPHIEinstalled on the OHP 1.93-m telescope. Characteristics and performancesof the spectrograph are presented, as well as the SOPHIE exoplanetconsortium program. With a minimum mass of 14.3 {M}_Jup, an orbitalperiod of 465 days and an eccentricity of 0.067, HD 16760b seems to belocated just at the end of the mass distribution of giant planets, closeto the planet/brown-dwarf transition. Its quite circular orbit supportsa formation in a gaseous protoplanetary disk.Based on observations made with SOPHIE spectrograph on the 1.93-mtelescope at Observatoire de Haute-Provence (CNRS/OAMP), France (program07A.PNP.CONS). Table 2 is also available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/505/853
| XID II: Statistical Cross-Association of ROSAT Bright Source Catalog X-ray Sources with 2MASS Point Source Catalog Near-Infrared Sources
The 18,806 ROSAT All Sky Survey Bright Source Catalog (RASS/BSC) X-raysources are quantitatively cross-associated with near-infrared (NIR)sources from the Two Micron All Sky Survey Point Source Catalog(2MASS/PSC). An association catalog is presented, listing the mostlikely counterpart for each RASS/BSC source, the probability Pid that the NIR source and X-ray source are uniquelyassociated, and the probability P no-id that none of the2MASS/PSC sources are associated with the X-ray source. The catalogincludes 3853 high quality (P id>0.98) X-ray-NIR matches,2280 medium quality (0.98 >= P id>0.9) matches, and4153 low quality (0.9 >= P id>0.5) matches. Of the highquality matches, 1418 are associations that are not listed in the SIMBADdatabase, and for which no high quality match with a USNO-A2 opticalsource was presented for the RASS/BSC source in previous work. Thepresent work offers a significant number of new associations withRASS/BSC objects that will require optical/NIR spectroscopy forclassification. For example, of the 6133 P id>0.92MASS/PSC counterparts presented in the association catalog, 2411 haveno classification listed in the SIMBAD database. These 2MASS/PSC sourceswill likely include scientifically useful examples of known sourceclasses of X-ray emitters (white dwarfs, coronally active stars, activegalactic nuclei), but may also contain previously unknown sourceclasses. It is determined that all coronally active stars in theRASS/BSC should have a counterpart in the 2MASS/PSC, and that the uniqueassociation of these RASS/BSC sources with their NIR counterparts thusis confusion limited.
| On the kinematic evolution of young local associations and the Scorpius-Centaurus complex
Context: Over the last decade, several groups of young (mainly low-mass)stars have been discovered in the solar neighbourhood (closer than ~100pc), thanks to cross-correlation between X-ray, optical spectroscopy andkinematic data. These young local associations - including an importantfraction whose members are Hipparcos stars - offer insights into thestar formation process in low-density environments, shed light on thesubstellar domain, and could have played an important role in the recenthistory of the local interstellar medium. Aims: To study the kinematicevolution of young local associations and their relation to other youngstellar groups and structures in the local interstellar medium, thuscasting new light on recent star formation processes in the solarneighbourhood. Methods: We compiled the data published in theliterature for young local associations. Using a realistic Galacticpotential we integrated the orbits for these associations and theSco-Cen complex back in time. Results: Combining these data with thespatial structure of the Local Bubble and the spiral structure of theGalaxy, we propose a recent history of star formation in the solarneighbourhood. We suggest that both the Sco-Cen complex and young localassociations originated as a result of the impact of the inner spiralarm shock wave against a giant molecular cloud. The core of the giantmolecular cloud formed the Sco-Cen complex, and some small cloudlets ina halo around the giant molecular cloud formed young local associationsseveral million years later. We also propose a supernova in young localassociations a few million years ago as the most likely candidate tohave reheated the Local Bubble to its present temperature.
| CCD astrometry and components instrumental magnitude difference of 432 Hipparcos wide visual double stars
Context: We measured the angular separations, position angles, ΔV, Δ y and Δ I of wide visual double stars during the period2003-2005. At least one component of the double stars in our sample hasan entry in the Hipparcos catalogue. Aims: Our measurements are acontribution to the study of the nature of these double stars. Methods: The northern double stars of the project were observed with the1.2 m telescope of the Kryonerion observatory and the southern with the1.0 m SAAO. We performed multiple-exposure CCD imaging of our targetsand used the standard procedure of data reduction and astrometric CCDcalibrations. Results: We present measurements of 213 northern and 219southern wide binaries.Based on observations made at Kryonerion Observatory of the NationalObservatory of Athens, Greece, and the South African AstronomicalObservatory. Full Table 1 and Tables 2, 3 are only available inelectronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/472/1055
| The Nearest Young Moving Groups
The latest results in the research of forming planetary systems have ledseveral authors to compile a sample of candidates for searching forplanets in the vicinity of the Sun. Young stellar associations areindeed excellent laboratories for this study, but some of them are notclose enough to allow the detection of planets through adaptive opticstechniques. However, the existence of very close young moving groups cansolve this problem. Here we have compiled the members of the nearestyoung moving groups, as well as a list of new candidates from ourcatalog of late-type stars that are possible members of young stellarkinematic groups, studying their membership through spectroscopic andphotometric criteria.
| Young Stars Near the Sun
Until the late 1990s the rich Hyades and the sparse UMa clusters werethe only coeval, comoving concentrations of stars known within 60 pc ofEarth. Both are hundreds of millions of years old. Then beginning in thelate 1990s the TW Hydrae Association, the Tucana/Horologium Association,the Pictoris Moving Group, and the AB Doradus Moving Group wereidentified within 60 pc of Earth, and the Chamaeleontis cluster wasfound at 97 pc. These young groups (ages 8 50 Myr), along with othernearby, young stars, will enable imaging and spectroscopic studies ofthe origin and early evolution of planetary systems.
| The AB Doradus Moving Group
From radio to X-ray wavelengths, AB Doradus has been an intensivelystudied star. We have identified ~30 nearby star systems, each with oneor more characteristics of youth, that are moving through space togetherwith AB Dor. This diverse set of ~50 million year old star systems isthe comoving, youthful group closest to Earth. The group's nucleus is aclustering of a dozen stars ~20 pc from Earth that includes AB Doritself. The AB Dor moving group joins the previously known and somewhatyounger and more distant Tucana/Horologium and TW Hydrae associationsand the β Pictoris moving group as excellent laboratories forinvestigations of forming planetary systems.
| GPM - compiled catalogue of absolute proper motions of stars in selected areas of sky with galaxies.
Not Available
| Maximum separations among cataloged binaries
The paper classifies many of the widest common-motion binaries listed inthe Aitken catalog and list 72 physical pairs with known photoelectricphotometry, 31 physical pairs without good photometry, and 27 opticalpairs. As a function of primary types, the physical systems have upperlimits to their separations that are exceeded by some of the opticalpairs. The fact that optical pairs occur with larger separations impliesthat the limits are real ones and not just catalog limitations. Thoselimits (in AU) are expressed by 2500 M1 exp 1.54 for B5-KO main-sequenceprimaries. The same limits hold for the Trapezium and hierarchicalsystems studied previously.
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Observation and Astrometry data
| Constellation: | ペルセウス座 |
| Right ascension: | 02h42m20.96s |
| Declination: | +38°37'21.3" |
| Apparent magnitude: | 10.276 |
| Distance: | 44.903 parsecs |
| Proper motion RA: | 81 |
| Proper motion Dec: | -105.4 |
| B-T magnitude: | 11.507 |
| V-T magnitude: | 10.378 |
Catalogs and designations:
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