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SCUBA observations of dust around Lindroos stars: evidence for a substantial submillimetre disc population
We have observed 22 young stars from the Lindroos sample at 850 μmwith SCUBA on the James Clerk Maxwell Telescope to search for evidenceof dust discs. Stars in this sample are the less massive companions ofB-type primaries and have well-defined ages that are 10- 170 Myr; i.e.they are about to, or have recently arrived on the main sequence. Dustwas detected around three of these stars (HD 112412, 74067 and 99803B).The emission around HD 74067 is centrally peaked and is approximatelysymmetrically distributed out to ~70 arcsec from the star. This emissionarises from either a two-component disc, one circumstellar and the othercircumbinary with dust masses of 0.3 and <27 M⊕,respectively, or an unrelated background object. The other twodetections we attribute to circumsecondary discs with masses of 0.04 and0.3 M⊕. We were also able to show that a circumprimarydisc is present around HD 112413 with a similar mass to that around thecompanion HD 112412. Cross-correlation of our sample with the IRAScatalogues only showed evidence for dust emission at 25 and 60 μmtoward one star (HD 1438); none of the submillimetre detections wereevident in the far-infrared data implying that these discs are cold(>40 K assuming β= 1). Our submillimetre detections are some ofthe first of dust discs surrounding evolved stars that were not detectedby IRAS or ISO and imply that 9-14 per cent of stars could harbourpreviously undetected dust discs that await discovery in unbiased sub-mmsurveys. If these discs are protoplanetary remnants, rather thansecondary debris discs, dust lifetime arguments show that they must bedevoid of small <0.1 mm grains. Thus it may be possible to determinethe origin of these discs from their spectral energy distributions. Thelow inferred dust masses for this sample support the picture thatprotoplanetary dust discs are depleted to the levels of the brightestdebris discs (~1 M⊕) within 10 Myr, although if theextended emission of HD 74067 is associated with the star, this wouldindicate that >10 M⊕ of circumbinary material canpersist until ~60 Myr and would also support the theory that T Tauridiscs in binary systems are replenished by circumbinary envelopes.
| A spectroscopic survey for lambda Bootis stars. II. The observational data
lambda Bootis stars comprise only a small number of all A-type stars andare characterized as nonmagnetic, Population i, late B to early F-typedwarfs which show significant underabundances of metals whereas thelight elements (C, N, O and S) are almost normal abundant compared tothe Sun. In the second paper on a spectroscopic survey for lambda Bootisstars, we present the spectral classifications of all program starsobserved. These stars were selected on the basis of their Strömgrenuvbybeta colors as lambda Bootis candidates. In total, 708 objects insix open clusters, the Orion OB1 association and the Galactic field wereclassified. In addition, 9 serendipity non-candidates in the vicinity ofour program stars as well as 15 Guide Star Catalogue stars were observedresulting in a total of 732 classified stars. The 15 objects from theGuide Star Catalogue are part of a program for the classification ofapparent variable stars from the Fine Guidance Sensors of the HubbleSpace Telescope. A grid of 105 MK standard as well as ``pathological''stars guarantees a precise classification. A comparison of our spectralclassification with the extensive work of Abt & Morrell(\cite{Abt95}) shows no significant differences. The derived types are0.23 +/- 0.09 (rms error per measurement) subclasses later and 0.30 +/-0.08 luminosity classes more luminous than those of Abt & Morrell(\cite{Abt95}) based on a sample of 160 objects in common. The estimatederrors of the means are +/- 0.1 subclasses. The characteristics of oursample are discussed in respect to the distribution on the sky, apparentvisual magnitudes and Strömgren uvbybeta colors. Based onobservations from the Observatoire de Haute-Provence, OsservatorioAstronomico di Padova-Asiago, Observatório do Pico dosDias-LNA/CNPq/MCT, Chews Ridge Observatory (MIRA) and University ofToronto Southern Observatory (Las Campanas).
| Determination of the relative positions of stars that are components of Trapezium-type multiple systems
A 125-cm automated mirror telescope with a Ritchey-Chretien opticalsystem was used to determine the relative positions of stars in 25Trapezium-type multiple systems. Distances and position angles for themean observational epochs are also given along with mean errors indetermining these distances and position angles.
| A study of visual double stars with early-type primaries. V - Post-T Tauri secondaries
In an ongoing study of companions of O and B type primaries, themajority of the secondaries are found to be of spectral type F, G, or K.Their properties are investigated in relation to their evolutionarystatus. The ages of the systems have been determined from uvby-betaphotometry of the primaries and it is found that all are younger than150 million years and half are less than 30 million years old.Thirty-seven secondaries have ages less than the expected contractiontime to the zero-age-main sequence (ZAMS). More than 50 percent of theF, G, and K secondaries exhibit spectroscopic features (Ca II H, K andH-alpha emission and strong Li absorption) typical of young stars andreminiscent of T Tauri stars although not as conspicuous. It isappropriate to classify them as post-T Tauri stars. The lifetime of somefeatures characteristic of early stellar evolution is discussed.
| A study of visual double stars with early type primaries. IV Astrophysical data
Astrophysical parameters (MK class, color excess, absolute magnitude,distance, effective temperature, mass, and age) are derived fromcalibrations of the uvby-beta indices for the members of 253 doublestars with O or B type primaries and faint secondaries. The photometricspectral classification is compared to the MK classes, and the agreementis very good. The derived data together with spectroscopic and JHKL dataare used for deciding which pairs are likely to be physical and whichare optical, and it is shown that 98 (34 percent) of the secondaries arelikely to be members of physical systems. For 90 percent of the physicalpairs the projected separation between the components is less than25,000 AU. A majority of the physical secondaries are late-type stars,and 50 percent of them are contracting towards the zero-agemain-sequence. Also presented are new uvby-beta data for 43 secondariesand a computer program for determining astrophysical parameters fromuvby-beta data.
| A study of visual double stars with early type primaries. II - Photometric results
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1983A&AS...51..161L&db_key=AST
| A study of visual double stars with early type primaries. I - Spectroscopic results
Attention is given to spectral peculiarities found in data on thespectral classes of 486 stars in 254 visual doublet or multiplet systemswith O or B type primaries, in order to isolate a group of very youngstars that may serve for the study of early stellar evolutioncharacteristics. It is noted that the material contains a substantialfraction of secondaries that are likely to be physical, and that severalof these may be in the premain-sequence phase of stellar evolution, orhave reached the zero-age main sequence.
| Photometric Study of Trapezium-Type Systems
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1979RMxAA...4..287E&db_key=AST
| UBVRI photometry of stars in Trapezium type systems.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977RMxAA...3..133W&db_key=AST
| The kinematics of trapezium systems.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974RMxAA...1..101A&db_key=AST
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Osservazione e dati astrometrici
| Costellazione: | Cane Minore |
| Ascensione retta: | 07h47m02.47s |
| Declinazione: | +00°01'06.1" |
| Magnitudine apparente: | 8.409 |
| Distanza: | 473.934 parsec |
| Moto proprio RA: | 1.6 |
| Moto proprio Dec: | -4.1 |
| B-T magnitude: | 8.377 |
| V-T magnitude: | 8.407 |
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