Pre-main sequence star Proper Motion Catalogue

Ducourant, C.; Teixeira, R.; Périé, J. P.; Lecampion, J. F.; Guibert, J.; Sartori, M. J.

doi:10.1051/0004-6361:20052788

Cited by 93 publications

(140 citation statements)

References 48 publications

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“…In Kohoutek & Wehmeyer (1997), brightness in the visual or photovisual color system (m pv = 17. m 0) and spectral type K6IVe is given. Ducourant et al (2005) Our measurements indicate the same range of V values as in Armond et al (2011), Cohen & Kuhi (1979, Kohoutek & Wehmeyer (1997), and Laugalys et al (2006), while mean magnitude in I band is for about 1 mag less. The R band displays least scatter of measurements, which are in accordance with the data of Armond et al (2011).…”

Section: Lkhα 189supporting

confidence: 76%

Long-term photometric observations of pre-main sequence objects in the field of North America/Pelican Nebula

Beljan

Jurdana-Šepić

Semkov

et al. 2014

A&A

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To broaden the search and study stars in the early evolutionary phase, we investigated a sample of 17 pre-main sequence objects previously detected as either Hα emission-line pre-main sequence stars or T Tauri variables located in the field of the North America/Pelican Nebula complex. Johnson-Cousins B, V, R c , I c magnitudes and mean color indices for the program stars are determined from more than 12 400 measurements from archive photographic plates and from CCD data collected at 7 observatories covering the period of almost 60 years from 1954 up to 2013. We complemented previously rare insights on the photometry of the program stars and presented their photometric history, which for almost all program stars is the first long term photometric monitoring on a timescale of 6 decades. Eight program stars are found to be classical T Tauri stars of variability type II, while 6 program stars are weak-line T Tauri stars of variability type I. For the first time, periodicity is found for three stars: V1716 Cyg indicates a 4.15 day period, V2051 Cyg indicates a 384 day period, and V521 Cyg a period of 503 days.

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Section: Lkhα 189supporting

confidence: 76%

Long-term photometric observations of pre-main sequence objects in the field of North America/Pelican Nebula

Beljan

Jurdana-Šepić

Semkov

et al. 2014

A&A

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“…13). They are two close (ρ ∼ 40 arcsec) pre-main sequence stars in the σ Orionis cluster that have appeared in a number of young and emission-line star catalogues (Herbig & Kameswara Rao 1972;Cohen & Kuhi 1979;Herbig & Bell 1988;Ducourant et al 2005). As in the case of many variable stars in this work, they were discovered as variable stars by Pickering (1904 Pickering (1906) and Haro & Moreno (1953), respectively.…”

Section: Ry Ori (No 11)mentioning

confidence: 53%

Finding the most variable stars in the Orion Belt with the All Sky Automated Survey

2010

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We look for high-amplitude variable young stars in the open clusters and associations of the Orion Belt. We use public data from the ASAS-3 Photometric V -band Catalogue of the All Sky Automated Survey, infrared photometry from the 2MASS and IRAS catalogues, proper motions, and the Aladin sky atlas to obtain a list of the most variable stars in a survey area of side 5 deg centred on the bright star Alnilam (ǫ Ori) in the centre of the Orion Belt. We identify 32 highly-variable stars, of which 16 had not been reported to vary before. They are mostly variable young stars and candidates (16) and background giants (8), but there are also field cataclysmic variables, contact binaries, and eclipsing binary candidates. Of the young stars, which typically are active Herbig Ae/Be and T Tauri stars with Hα emission and infrared flux excess, we discover four new variables and confirm the variability status of another two. Some of them belong to the well known σ Orionis cluster. Besides, six of the eight giants are new variables, and three are new periodic variables.

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“…Li & Hu (1998) considered this star as WTTS candidate with spectral type G5IV. Also considered as PMS in the Ducourant et al (2005) catalogue. -RasTyc 0348+5202: quoted as a double or multiple G6IV star (Bartkevičius & Gudas 2002) while classified as K0V in Jacoby et al (1984) spectral atlas.…”

Section: Discussionmentioning

confidence: 99%

A spectroscopic survey of the youngest field stars in the solar neighbourhood

Guillout¹,

Klutsch²,

Frasca

et al. 2009

A&A

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Aims. We present the first results of an ambitious ground-based observation programme conducted on 1-4 meter class telescopes. Our sample consists of 1097 active and presumably young stars, all of them being optical (Tycho Catalogue) counterparts of ROSAT All-Sky Survey X-ray sources in the northern hemisphere. In this paper, we concentrate on the optically brightest (V T 9. m 5) candidates (704 objects). We acquired high-resolution optical spectroscopy in the Hα and/or lithium spectral regions for 426 of such stars without relevant data in the literature. We describe the star sample and the observations and we start to discuss the physical properties of the investigated stars. Methods. We used a cross-correlation technique and other tools developed by us to derive accurate radial and rotational velocities and to perform an automatic spectral classification for both single stars and double-lined systems. The spectral subtraction technique was used to derive chromospheric activity levels and lithium abundances. We estimated the fraction of young single stars and multiple systems in stellar soft X-ray surveys and the contamination by more evolved systems, like RS CVn binaries. We classified stars on the basis of their lithium abundance and give a glimpse of their sky distribution.Results. The sample appears to be a mixture of quite young Pleiades-like and Hyades-like stars plus an older lithium-poor population probably born within the last 1-2 Gyr. Seven stars with a lithium abundance compatible with the age of IC 2602 (about 30 Myr) or even younger were detected as well, although two appear to be lithium-rich giants.The discovery of a large number of highly or moderately lithium-rich giants is another outcome of the present survey. Conclusions. The contamination of soft X-ray surveys by old systems in which the activity level is enhanced by tidal synchronisation is not negligible, especially for K-type stars. Five stars with lithium content close to the primordial abundance are probably associated with already known moving groups in the solar neighbourhood. Some of them are good post-T Tauri candidates according to their positions in the HR diagram.

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Pre-main sequence star Proper Motion Catalogue

Cited by 93 publications

References 48 publications

Long-term photometric observations of pre-main sequence objects in the field of North America/Pelican Nebula

Long-term photometric observations of pre-main sequence objects in the field of North America/Pelican Nebula

Finding the most variable stars in the Orion Belt with the All Sky Automated Survey

A spectroscopic survey of the youngest field stars in the solar neighbourhood

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