Young Stars with SALT*

Riedel, Adric R.; Alam, Munazza K.; Rice, Emily L.; Cruz, Kelle L.; Henry, Todd J.

doi:10.3847/1538-4357/840/2/87

Cited by 37 publications

(32 citation statements)

References 63 publications

(77 reference statements)

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“…• 12 pre-main sequence stellar systems that are identified to be part of the AB Doradus (two systems), Argus (three system), Tucana-Horologium (5), β Pictoris (1), and TW Hydra (1) moving groups, plus two additional stars that do not appear to be associated with any group. The unassociated stars (along with other young non-members identified in Riedel et al 2014 andRiedel et al 2017a) hint at a complex outcome to the star formation process that yields relatively young stars that cannot be straightforwardly linked to known assocations or moving groups.…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

The Solar Neighborhood. XLIII. Discovery of New Nearby Stars with μ < 0.″18 yr⁻¹ (TINYMO Sample)

Riedel

Silverstein

Henry³

et al. 2018

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We have conducted a novel search of most of the southern sky for nearby red dwarfs having low proper motions, with specific emphasis on those with µ < 0. ′′ 18 yr −1 , the lower cutoff of Luyten's classic proper motion catalog. We used a tightly constrained search of the SuperCOSMOS database and a suite of photometric distance relations for photographic BRI and 2MASS JHK s magnitudes to estimate distances to more than fourteen million red dwarf candidates. Here we discuss 29 stars in 26 systems estimated to be within 25 parsecs, all of which have µ <0. ′′ 18 yr −1 , which we have investigated using milliarcsecond astrometry, V RI photometry, and low-resolution spectroscopy. In total, we present the first parallaxes of 20 star systems, nine of which are within 25 parsecs. We have additionally identified eight young M dwarfs, of which two are new members of the nearby young moving groups, and 72 new giants, including two new carbon stars. We also present the entire catalog of 1215 sources we have identified by this means.

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Section: Discussionmentioning

confidence: 99%

“…The TINYMO survey contains a large number of nearby young stars, (55, counting Riedel et al 2014, Riedel et al 2017a, and this paper) where they make up perhaps 4% of all stars (Riedel et al 2017b). There are two primary reasons for this.…”

Section: Why So Many Young Stars?mentioning

confidence: 99%

The Solar Neighborhood. XLIII. Discovery of New Nearby Stars with μ < 0.″18 yr⁻¹ (TINYMO Sample)

Riedel

Silverstein

Henry³

et al. 2018

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“…Delfosse et al 1998;Mohanty & Basri 2003;Reiners et al 2012;West et al 2015;Newton et al 2017). Furthermore, several studies have extended the idea that magnetic activity decreases with age for late-M dwarfs (Fleming et al 1995;Eggen 1990;West et al 2006West et al , 2008aRiedel et al 2017). This indicates that there is an empirical relation between age, rotation and magnetic activity for M dwarfs that may extend to L dwarfs as well.…”

Section: Introductionmentioning

confidence: 89%

Exploring the Age-dependent Properties of M and L Dwarfs Using Gaia and SDSS

Kiman

Schmidt

Angus

et al. 2019

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109

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We present a sample of 74, 216 M and L dwarfs a) constructed from two existing catalogs of cool dwarfs spectroscopically identified in the Sloan Digital Sky Survey (SDSS). We cross-matched the SDSS catalog with Gaia DR2 to obtain parallaxes and proper motions and modified the quality cuts suggested by the Gaia Collaboration to make them suitable for late-M and L dwarfs. We also provide relations between Gaia colors and absolute magnitudes with spectral type and conclude that (G − G RP ) has the tightest relation to spectral type for M and L dwarfs. In addition, we study magnetic activity as a function of position on the color-magnitude diagram, finding that Hα magnetically active stars have, on average, redder colors and/or brighter magnitudes than inactive stars. This effect cannot be explained by youth alone and might indicate that active stars are magnetically inflated, binaries and/or high metallicity. Moreover, we find that vertical velocity and vertical action dispersion are correlated with Hα emission, confirming that these two parameters are age indicators. We also find that stars below the main sequence have high tangential velocity which is consistent with a low metallicity and old population of stars that belong to the halo or thick disk.

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“…K -GJ 2006A is part of a common proper motion visual binary (Riedel et al 2014(Riedel et al , 2017 at a distance of 34.8 pc. Both components are of spectral type M3.5Ve, with A being brighter than B with respective magnitudes B A = 14.33 and B B = 14.66 (Zacharias et al 2012).…”

Section: G -αmentioning

confidence: 99%

EMISSA (Exploring Millimeter Indicators of Solar-Stellar Activity)

Mohan

Wedemeyer

Pandit

et al. 2021

A&A

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Context. Due to their wide wavelength coverage across the millimeter to centimeter (mm–cm) range and their increased sensitivity, modern interferometric arrays facilitate observations of the thermal and non-thermal radiation that is emitted from different layers in the outer atmospheres of stars. Aims. We study the spectral energy distribution (Sobs(ν)) of main-sequence stars based on archival observations in the mm–cm range with the aim to study their atmospheric stratification as a function of stellar type. Methods. The main-sequence stars with significant detection in mm bands were identified in the ALMA Science Archive. These data were then complemented with spectral flux data in the extreme ultraviolet to cm range as compiled from various catalogues and observatory archives. We compared the resultant Sobs(ν) of each star with a photospheric emission model (Smod(ν)) calculated with the PHOENIX code. The departures of Sobs(ν) from Smod(ν) were quantified in terms of a spectral flux excess parameter (ΔS∕Smod) and studied as a function of stellar type. Results. The initial sample consists of 12 main-sequence stars across a broad range of spectral types from A1 to M3.5 and the Sun-as-a-star as reference. The stars with Teff = 3000–7000 K (F–M type) showed a systematically higher Sobs(ν) than Smod(ν) in the mm–cm range. Their ΔS∕Smod exhibits a monotonic rise with decreasing frequency. The steepness of this rise is higher for cooler stars in the Teff = 3000–7000 K range, although the single fully convective star (Teff ~ 3000 K) in the sample deviates from this trend. Meanwhile, Sobs(ν) of the A-type stars agrees with Smod(ν) within errors. Conclusions. The systematically high ΔS∕Smod in F–M stars indicates hotter upper atmospheric layers, that is, a chromosphere and corona in these stars, like for the Sun. The mm–cm ΔS∕Smod spectrum offers a way to estimate the efficiency of the heating mechanisms across various outer atmospheric layers in main-sequence stars, and thereby to understand their structure and activity. We emphasise the need for dedicated surveys of main-sequence stars in the mm–cm range.

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Young Stars with SALT*

Cited by 37 publications

References 63 publications

The Solar Neighborhood. XLIII. Discovery of New Nearby Stars with μ < 0.″18 yr⁻¹ (TINYMO Sample)

The Solar Neighborhood. XLIII. Discovery of New Nearby Stars with μ < 0.″18 yr⁻¹ (TINYMO Sample)

Exploring the Age-dependent Properties of M and L Dwarfs Using Gaia and SDSS

EMISSA (Exploring Millimeter Indicators of Solar-Stellar Activity)

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Young Stars with SALT*

Cited by 37 publications

References 63 publications

The Solar Neighborhood. XLIII. Discovery of New Nearby Stars with μ < 0.″18 yr−1 (TINYMO Sample)

The Solar Neighborhood. XLIII. Discovery of New Nearby Stars with μ < 0.″18 yr−1 (TINYMO Sample)

Exploring the Age-dependent Properties of M and L Dwarfs Using Gaia and SDSS

EMISSA (Exploring Millimeter Indicators of Solar-Stellar Activity)

Contact Info

Product

Resources

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The Solar Neighborhood. XLIII. Discovery of New Nearby Stars with μ < 0.″18 yr⁻¹ (TINYMO Sample)

The Solar Neighborhood. XLIII. Discovery of New Nearby Stars with μ < 0.″18 yr⁻¹ (TINYMO Sample)