Spectroscopic confirmation of M-dwarf candidate members of the Beta Pictoris and AB Doradus Moving Groups

Binks, A. S.; Jeffries, R. D.

doi:10.1093/mnras/stv2431

Cited by 63 publications

(61 citation statements)

References 78 publications

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“…The star: β Pictoris is a bright (V = 3.85; Crifo et al 1997), southern (α = 05h47m17.08769s δ = −51 • 03 59.4412 ), nearby (d = 19.44 ± 0.05 pc; van Leeuwen 2007), young (23 ± 3 Myr; Mamajek & Bell 2014;Binks & Jeffries 2016), hot star (T eff = 8052 K; A6V; Gray et al 2006). The star has been reported to have δ Scuti like pulsations (Koen et al 2003).…”

Section: β Pictoris B and The Inferior Conjunction Of 2017mentioning

confidence: 99%

bRing: An observatory dedicated to monitoring the β Pictoris b Hill sphere transit

Stuik

Bailey

Dorval

et al. 2017

A&A

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Aims. We describe the design and first light observations from the β Pictoris b Ring ("bRing") project. The primary goal is to detect photometric variability from the young star β Pictoris due to circumplanetary material surrounding the directly imaged young extrasolar gas giant planet β Pictoris b. Methods. Over a nine month period centred on September 2017, the Hill sphere of the planet will cross in front of the star, providing a unique opportunity to directly probe the circumplanetary environment of a directly imaged planet through photometric and spectroscopic variations. We have built and installed the first of two bRing monitoring stations (one in South Africa and the other in Australia) that will measure the flux of β Pictoris, with a photometric precision of 0.5% over 5 min. Each station uses two wide field cameras to cover the declination of the star at all elevations. Detection of photometric fluctuations will trigger spectroscopic observations with large aperture telescopes in order to determine the gas and dust composition in a system at the end of the planet-forming era. Results. The first three months of operation demonstrate that bRing can obtain better than 0.5% photometry on β Pictoris in five minutes and is sensitive to nightly trends enabling the detection of any transiting material within the Hill sphere of the exoplanet.

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Section: β Pictoris B and The Inferior Conjunction Of 2017mentioning

confidence: 99%

bRing: An observatory dedicated to monitoring the β Pictoris b Hill sphere transit

Stuik

Bailey

Dorval

et al. 2017

A&A

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“…This system was found by Schlieder et al (2012) to be likely member of the association. However, the membership has been recently rejected by Binks & Jeffries (2016). It was photometrically monitored by the ASAS (ASAS 003235+0729.5) and NSVS (ID 9141792).…”

Section: Catalog Descriptionmentioning

confidence: 99%

“…This configuration may be an explanation of the measured relatively modest orbital rate. The membership has been recently rejected by Binks & Jeffries (2016). The first rotation period determination, P = 4.5 d, was reported by Gahm et al (1993) with the warning that it needed confirmation, since the star was observed for a time span of only six days.…”

Section: -2mass J05241914-1601153mentioning

confidence: 99%

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TheβPictoris association: Catalog of photometric rotational periods of low-mass members and candidate members

Messina

Millward²,

Buccino

et al. 2017

A&A

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Aims. We intended to compile the most complete catalog of bona fide members and candidate members of the β Pictoris association, and to measure their rotation periods and basic properties from our own observations, public archives, and exploring the literature. Methods. We carried out a multi-observatories campaign to get our own photometric time series and collected all archived public photometric data time series for the stars in our catalog. Each time series was analyzed with the Lomb-Scargle and CLEAN periodograms to search for the stellar rotation periods. We complemented the measured rotational properties with detailed information on multiplicity, membership, and projected rotational velocity available in the literature and discussed star by star. Results. We measured the rotation periods of 112 out of 117 among bona fide members and candidate members of the β Pictoris association and, whenever possible, we also measured the luminosity, radius, and inclination of the stellar rotation axis. This represents to date the largest catalog of rotation periods of any young loose stellar association. Conclusions. We provided an extensive catalog of rotation periods together with other relevant basic properties useful to explore a number of open issues, such as the causes of spread of rotation periods among coeval stars, evolution of angular momentum, and lithium-rotation connection.

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“…Recently there have been many works focussed on identifying the lower mass members of the young associations e.g. Shkolnik et al (2012), Schlieder et al (2012b), Rodriguez et al (2013), Malo et al (2014), Kraus et al (2014), A&A 590, A13 (2016) Gagné et al (2015), Binks & Jeffries (2016). Again, these surveys use a variety of techniques, however, the initial samples of low-mass candidate members are usually built upon multiplecatalogue photometry combined with proper motions.…”

Section: Introductionmentioning

confidence: 99%

Search for associations containing young stars (SACY)

Elliott

Bayo

Melo

et al. 2016

A&A

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Context. The young associations offer us one of the best opportunities to study the properties of young stellar and substellar objects and to directly image planets thanks to their proximity (<200 pc) and age (≈5−150 Myr). However, many previous works have been limited to identifying the brighter, more active members (≈1 M ) owing to photometric survey sensitivities limiting the detections of lower mass objects. Aims. We search the field of view of 542 previously identified members of the young associations to identify wide or extremely wide (1000−100 000 au in physical separation) companions. Methods. We combined 2MASS near-infrared photometry (J, H, K) with proper motion values (from UCAC4, PPMXL, NOMAD) to identify companions in the field of view of known members. We collated further photometry and spectroscopy from the literature and conducted our own high-resolution spectroscopic observations for a subsample of candidate members. This complementary information allowed us to assess the efficiency of our method. Results. We identified 84 targets (45: 0.2−1.3 M , 17: 0.08−0.2 M , 22: <0.08 M ) in our analysis, ten of which have been identified from spectroscopic analysis in previous young association works. For 33 of these 84, we were able to further assess their membership using a variety of properties (X-ray emission, UV excess, H α , lithium and K I equivalent widths, radial velocities, and CaH indices). We derive a success rate of 76-88% for this technique based on the consistency of these properties. Conclusions. Once confirmed, the targets identified in this work would significantly improve our knowledge of the lower mass end of the young associations. Additionally, these targets would make an ideal new sample for the identification and study of planets around nearby young stars. Given the predicted substellar mass of the majority of these new candidate members and their proximity, high-contrast imaging techniques would facilitate the search for new low-mass planets.

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Spectroscopic confirmation of M-dwarf candidate members of the Beta Pictoris and AB Doradus Moving Groups

Cited by 63 publications

References 78 publications

bRing: An observatory dedicated to monitoring the β Pictoris b Hill sphere transit

bRing: An observatory dedicated to monitoring the β Pictoris b Hill sphere transit

TheβPictoris association: Catalog of photometric rotational periods of low-mass members and candidate members

Search for associations containing young stars (SACY)

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