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A STELLAR CENSUS OF THE TUCANA-HOROLOGIUM MOVING GROUP
Open accessAbstract
We report the selection and spectroscopic confirmation of 129 new late-type (SpT = K3–M6) members of the Tucana–Horologium moving group, a nearby ( d ∼ 40 pc), young (τ ∼ 40 Myr) population of comoving stars. We also report observations for 13 of the 17 known Tuc–Hor members in this spectral type range, and that 62 additional candidates are likely to be unassociated field stars; the confirmation frequency for new candidates is therefore 129/191 = 67%. We have used radial velocities, Hα emission, and Li 6708 absorption to distinguish between contaminants and bona fide members. Our expanded census of Tuc–Hor increases the known population by a factor of ∼3 in total and by a factor of ∼8 for members with SpT ⩾ K3, but even so, the K–M dwarf population of Tuc–Hor is still markedly incomplete. Our expanded census allows for a much more detailed study of Tuc–Hor than was previously feasible. The spatial distribution of members appears to trace a two-dimensional sheet, with a broad distribution in X and Y , but a very narrow distribution (±5 pc) in Z . The corresponding velocity distribution is very small, with a scatter of ±1.1 km s −1 about the mean UVW velocity for stars spanning the entire 50 pc extent of Tuc–Hor. We also show that the isochronal age (τ ∼ 20–30 Myr) and the lithium depletion boundary age (τ ∼ 40 Myr) disagree, following the trend in other pre-main-sequence populations for isochrones to yield systematically younger ages. The Hα emission line strength follows a trend of increasing equivalent width with later spectral type, as is seen for young clusters. We find that moving group members have been depleted of measurable lithium for spectral types of K7.0–M4.5. None of our targets have significant infrared excesses in the WISE W3 band, yielding an upper limit on warm debris disks of F < 0.7%. Finally, our purely kinematic and color–magnitude selection procedure allows us to test the efficiency and completeness for activity-based selection of young stars. We find that 60% of K–M dwarfs in Tuc–Hor do not have ROSAT counterparts and would have been omitted in X-ray-selected samples. In contrast, GALEX UV-selected samples using a previously suggested criterion for youth achieve completeness of 77% and purity of 78%, and we suggest new SpT-dependent selection criteria that will yield >95% completeness for τ ∼ 40 Myr populations with GALEX data available.
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Citations
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Pecaut, M. J., & Mamajek, E. E. (2013) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/208/1/9 · Cited by 2,407 · cited 2×
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A SURVEY OF STELLAR FAMILIES: MULTIPLICITY OF SOLAR-TYPE STARS
Raghavan, D., McAlister, H. A., Henry, T. J., Latham, D. W., Marcy, G. W., Mason, B. D., Gies, D. R., White, R. J., & ten Brummelaar, T. A. (2010) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/190/1/1 · Cited by 1,922 · cited 1×
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BackgroundDirect Imaging of Multiple Planets Orbiting the Star HR 8799
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Cited by
Sorted by citations
Items 101–199 of 199
HERSCHEL OBSERVATIONS OF DUSTY DEBRIS DISKS
Vican, L., Schneider, A., Bryden, G., Melis, C., Zuckerman, B., Rhee, J., & Song, I. (2016) · The Astrophysical Journal · doi:10.3847/1538-4357/833/2/263 · Cited by 29
“This relatively high fractional IR luminosity is surprising, given its 300 Myr age.”
BackgroundInfluentialCorrecting For Telluric Absorption: Methods, Case Studies, And Release Of The TelFit Code
Kraus, A. (2016) · Texas ScholarWorks (Texas Digital Library) · doi:10.15781/t2mv4s · Cited by 28
Self-citationA Pre-Gaia Census of Nearby Stellar Groups
Mamajek, E. E. (2015) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921315006250 · Cited by 28
“K7-M5 Tuc-Hor members from Kraus et al. (2014) projected within its estimated tidal radius 2.8 pc ∼3◦.7: 2MASS J01344601-5707564, J01375879-5645447, J01504543-5716488, J01380311-5904042, J01505688-5844032, J01521830-5950168, J01275875-6032243.”
BackgroundMethodInfluentialInsights into star formation and dispersal from the synchronization of stellar clocks
Miret-Roig, N., Alves, J., Barrado, D., Burkert, A. M., Ratzenböck, S., & Konietzka, R. (2023) · Nature Astronomy · doi:10.1038/s41550-023-02132-4 · Cited by 28
“The Tuc–Hor association is located at around 47 pc and has an age of 30–50 Myr from isochrone-fitting 78,83 , dynamics 38,40 and the LDB approach 27,81,84 .”
Binks, A. S., Jeffries, R. D., & Maxted, P. F. L. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1309 · Cited by 28
Shkolnik, E. L., Rolph, K. A., Peacock, S., & Barman, T. S. (2014) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/796/1/l20 · Cited by 27
“In order to gain access to the Lyα emission of many more stars than is currently possible to observe (i.e., with HST), we sought 7 Note that the strongest UV emitting M star in the sample is the young Speedy Mic (40 Myr; Kraus et al. 2014) and the weakest emitting is the old GJ 876.”
Self-citationKepler and the Behemoth: Three Mini-Neptunes in a 40 Million Year Old Association
Bouma, L. G., Kerr, R. M. P., Curtis, J. L., Isaacson, H. T., Hillenbrand, L. A., Howard, A. W., Kraus, A. L., Bieryla, A., Latham, D. W., Petigura, E. A., et al. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac93ff · Cited by 26
“Kraus et al. (2014) for instance, in their survey of Tuc-Hor (≈40 Myr), observed that all cluster members with spectral types >K4.”
BackgroundSelf-citationSchulreich, M. M., Feige, J., & Breitschwerdt, D. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347532 · Cited by 25
Effective Temperatures of Low-mass Stars from High-resolution H-band Spectroscopy
López–Valdivia, R., Mace, G. N., Sokal, K. R., Hussaini, M., Kidder, B. T., Mann, A. W., Gosnell, N. M., Oh, H., Kesseli, A. Y., Muirhead, P. S., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab2129 · Cited by 25
New members of the TW Hydrae Association and two accreting M-dwarfs in Scorpius–Centaurus
Murphy, S. J., Lawson, W. A., & Bento, J. D. S. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1745 · Cited by 24
Li in Open Clusters: Cool Dwarfs in the Young, Subsolar-metallicity Cluster M35 (NGC 2168)*
Anthony-Twarog, B. J., Deliyannis, C. P., Harmer, D., Lee-Brown, D. B., Steinhauer, A., Sun, Q., & Twarog, B. A. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aacb1f · Cited by 24
Dynamical age of the Tucana-Horologium young stellar association
Galli, P. A. B., Miret-Roig, N., Bouy, H., Olivares, J., & Barrado, D. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad520 · Cited by 23
Hayward, T. L. (2016) · Figshare · doi:10.15781/t25r6g · Cited by 23
A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Bouma, L. G., Curtis, J. L., Masuda, K., Hillenbrand, L. A., Stefánsson, G., Isaacson, H. T., Narita, N., Fukui, A., Ikoma, M., Tamura, M., et al. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac4966 · Cited by 22
Self-citationStellar population of the Rosette Nebula and NGC 2244
Mužić, K., Almendros-Abad, V., Bouy, H., Kubiak, K., Ramírez, K. P., Krone-Martins, A., Moitinho, A., & Conceição, M. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243659 · Cited by 22
SPYGLASS. II. The Multigenerational and Multiorigin Star Formation History of Cepheus Far North
Kerr, R. M. P., Kraus, A. L., Murphy, S. J., Krolikowski, D. M., Offner, S. S. R., Tofflemire, B. M., & Rizzuto, A. C. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac9b45 · Cited by 22
“The choice of age zero-point within commonly used options has a negligible effect on reported ages (of order 0.01 Myr; see Murphy et al. 2021 for a discussion), whereas larger systematic uncertainties exist through the use of non-rotating models (Murphy et al. 2022).”
ResultInfluentialSelf-citationThe Multiplicity of M Dwarfs in Young Moving Groups
Shan, Y., Yee, J. C., Bowler, B. P., Cieza, L. A., Montet, B. T., Cánovas, H., Liu, M. C., Close, L. M., Hinz, P. M., Males, J. R., et al. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa859d · Cited by 22
“Our target list is drawn primarily from Malo et al. 2013, 2014 (64 targets), and Kraus et al. 2014 (34 targets), and supplemented by targets from Moór et al. 2013 (5 targets) and Rodriguez et al. 2013 (2 targets).”
BackgroundMethodInfluentialSelf-citationNew binaries from the SHINE survey
Bonavita, M., Gratton, R., Desidera, S., Squicciarini, V., D’Orazi, V., Zurlo, A., Biller, B. A., Chauvin, G., Fontanive, C., Janson, M., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202140510 · Cited by 21
Hawkins, K., Lucey, M., & Curtis, J. L. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1673 · Cited by 21
“Furthermore, the 3D velocity dispersion (1.3 km s−1, though this value is limited by the Gaia DR2 RV errors), is on the order of other known OB associations (Tuc–Hor: 1.1 km s−1; Kraus et al. 2014).”
BackgroundInfluentialRichey-Yowell, T., Shkolnik, E. L., Loyd, R. O. P., Jackman, J. A. G., Schneider, A. C., Agüeros, M. A., Barman, T., Meadows, V., Gibson, R., & Douglas, S. T. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac5f48 · Cited by 20
“The young star sample of 10 K stars was taken from the TucanaHorologium young moving group (40± 5Myr; Kraus et al. 2014) and confirmed to be bona fide members through their 3D space velocity motions and lithium depletion by Kraus et al. Similarly, our intermediate stellar sample of 15 K stars was…”
BackgroundMethodSelf-citationMeshkat, T., Kenworthy, M. A., Reggiani, M., Quanz, S. P., Mamajek, E. E., & Meyer, M. R. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1779 · Cited by 20
“Except for one,1 our targets are all members of nearby young moving groups or associations: β Pic Moving Group (23 ± 3 Myr; Mamajek & Bell 2014), Tuc-Hor Association (40 Myr; Kraus et al. 2014), AB Dor Association (125 ± 15 Myr; Barenfeld et al. 2013).”
BackgroundMethodInfluentialBayesian assessment of moving group membership: importance of models and prior knowledge
Lee, J., & Song, I. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx3195 · Cited by 20
A Mid-infrared Study of Directly Imaged Planetary-mass Companions Using Archival Spitzer/IRAC Images
Martinez, R. A., & Kraus, A. L. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/ac3745 · Cited by 20
“AB Pic is a K2 star originally considered a member of the Tucana–Horologium association (τ∼ 40Myr; Song et al. 2003; Kraus et al. 2014b; Bell et al. 2015).”
BackgroundResultInfluentialSelf-citationShort-term variability of DS Tucanae A observed with TESS
Colombo, S., Petralia, A., & Micela, G. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243086 · Cited by 20
A Population of Dipper Stars from the Transiting Exoplanet Survey Satellite Mission
Capistrant, B. K., Soares-Furtado, M., Vanderburg, A. M., Kounkel, M., Rappaport, S., Omohundro, M., Powell, B. P., Gagliano, R., Jacobs, T. L., Kostov, V. B., et al. (2022) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ac9125 · Cited by 19
“To determine the IR excess, we combined the data from Pecaut & Mamajek (2013) and Kraus et al. (2014), establishing an expected baseline W1 – W3 color for young stellar sources (<50 Myr).”
MethodHAZMAT. IX. An Analysis of the UV and X-Ray Evolution of Low-mass Stars in the Era of Gaia
Richey-Yowell, T., Shkolnik, E. L., Schneider, A. C., Peacock, S., Huseby, L., Jackman, J. A. G., Barman, T., Osby, E., & Meadows, V. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acd2dc · Cited by 20
“…(24± 3Myr; Zuckerman et al. 2001; Shkolnik et al. 2017), Columba (42- + 4 6 Myr; Torres et al. 2008; Bell et al. 2015), Tucana-Horologium (45± 4Myr; Kraus et al. 2014; Bell et al. 2015), AB Doradus (149- + 19 51 Myr; Zuckerman et al. 2004; Bell et al. 2015), Ursa Majoris (414± 23 Myr; Eggen…”
Self-citationZuckerman, B., Klein, B., & Kastner, J. H. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab45ea · Cited by 19
WEIRD: Wide-orbit Exoplanet Search with InfraRed Direct Imaging
Baron, F., Artigau, É., Rameau, J., Lafreniére, D., Gagné, J., Malo, L., Albert, L., Naud, M.-È., Doyon, R., Janson, M., et al. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aad599 · Cited by 21
“…& Simon 2009; Shkolnik et al. 2009, 2012; Schlieder et al. 2010, 2012a, 2012b; Kiss et al. 2011; Rodriguez et al. 2011; Liu et al. 2013; Malo et al. 2013, 2014; Moór et al. 2013; Rodriguez et al. 2013; Kraus et al. 2014; Riedel et al. 2014; Gagné et al. 2014; Binks et al. 2015; Gagné et al. 2015b).”
Galli, P. A. B., Bouy, H., Olivares, J., Miret-Roig, N., Sarro, L. M., Barrado, D., & Berihuete, Á. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202141366 · Cited by 17
Wang, F., Fang, M., Fu, X., Chen, Y., Li, L., Pang, X., Li, Z., Tang, J., Cui, W., Tian, H., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ad960a · Cited by 18
Dust cleansing of star-forming gas
Gustafsson, B. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833353 · Cited by 16
“Kraus et al. (2014), on the basis of IR observations, find an upper limit of 5% on the fraction of K3.”
BackgroundMultiplicity of stars with planets in the solar neighbourhood
González-Payo, J., Caballero, J. A., Gorgas, J., Cortés‐Contreras, M., Gálvez-Ortiz, M. C., & Cifuentes, C. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202450048 · Cited by 15
CARMENES input catalogue of M dwarfs
Cortés‐Contreras, M., Caballero, A., Montes, D., Guillén, C. C., Béjar, V. J. S., Cifuentes, C., Tabernero, M., Osorio, M. R. Z., Amado, J. P., Jeffers, S. V., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202451585 · Cited by 15
Hinkley, S., Matthews, E. C., Lefèvre, C., Lestrade, J., Kennedy, G., Mawet, D. P., Stapelfeldt, K. R., Ray, S., Mamajek, E. E., Bowler, B. P., et al. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abec6e · Cited by 15
“…form the majority of the population of these groups, but have only begun to be identified in large numbers in the last several years, partly with the arrival of kinematic data from the Gaia mission (e.g. Kraus et al. 2014; Gagné & Faherty 2018; Gaia Collaboration et al. 2018; Bowler et al. 2019).”
BackgroundEvryFlare. iv. Detection of Periodicity in Flare Occurrence from Cool Stars with TESS
Howard, W. S., & Law, N. M. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac142a · Cited by 14
Supernova ejecta in ocean cores used as time constraints for nearby stellar groups
Hyde, M., & Pecaut, M. J. (2017) · Astronomische Nachrichten · doi:10.1002/asna.201713375 · Cited by 14
“Tuc-Hor is the largest young moving group of stars nearby, making it an excellent SN progenitor host association, with a distance of ∼40pc away (Kraus et al. 2014; Zuckerman et al. 2001).”
BackgroundBinaries among low-mass stars in nearby young moving groups
Janson, M., Durkan, S., Hippler, S., Dai, X., Brandner, W., Schlieder, J. E., Bonnefoy, M., & Henning, T. K. (2017) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201629945/pdf · Cited by 13
Low-mass members of nearby young stellar moving groups from Gaia EDR3
Lee, J., Song, I., & Murphy, S. J. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac358 · Cited by 12
A Census of the β Pic Moving Group and Other Nearby Associations with Gaia*
Luhman, K. L. (2024) · The Astronomical Journal · doi:10.3847/1538-3881/ad697d · Cited by 15
Herschel Observations of Disks around Late-type Stars
Tanner, A., Plavchan, P., Bryden, G., Kennedy, G., Matrá, L., Cronin-Coltsmann, P. F., Lowrance, P., Henry, T., Riaz, B., Gizis, J., et al. (2020) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/ab895f · Cited by 7
The binary system of the spinning-top Be star Achernar
Kervella, P., Borgniet, S., de Souza, A. D., Mérand, A., Gallenne, A., Rivinius, T., Lacour, S., Carciofi, A. C., Faes, D. M., Bouquin, J.-B. L., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244009 · Cited by 12
TIC 278956474: Two Close Binaries in One Young Quadruple System Identified by TESS
Rowden, P., Borkovits, T., Jenkins, J. M., Stassun, K. G., Twicken, J. D., Newton, E. R., Ziegler, C., Hellier, C., Soto, A. G., Matthews, E. C., et al. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/ab9d20 · Cited by 12
TIC 278956474: Two Close Binaries in One Young Quadruple System Identified by TESS
Rowden, P., Borkovits, T., Jenkins, J. M., Stassun, K. G., Twicken, J. D., Newton, E. R., Ziegler, C., Hellier, C., Soto, A. G., Matthews, E. C., et al. (2020) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · Cited by 12
Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Sanghi, A., Xuan, J. W., Wang, J. J., Mawet, D., Bowler, B. P., Ngo, H., Bryan, M., Ruane, G., Absil, O., & Huby, E. (2024) · Astronomical Journal · doi:10.3847/1538-3881/ad769f · Cited by 14
Examining the Rotation Period Distribution of the 40 Myr Tucana–Horologium Association with TESS
Popinchalk, M., Faherty, J. K., Curtis, J. L., Gagné, J., Gagliuffi, D. C. B., Vos, J. M., Ayala, A., Quevedo, L. G., & Kiman, R. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acb055 · Cited by 11
“For a moving group like Tuc-Hor, TESS provides the ideal data set to collect rotation periods from F stars down into the M-dwarf regime.”
BackgroundMethodResultInfluentialReaching the boundary between stellar kinematic groups and very wide binaries
González-Payo, J., Caballero, J. A., & Cortés‐Contreras, M. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202245476 · Cited by 10
Banyan. X. Discovery of a Wide, Low-gravity L-type Companion to a Fast-rotating M3 Dwarf*
Desrochers, M. E., Artigau, É., Gagné, J., Doyon, R., Malo, L., Faherty, J. K., & Lafreniére, D. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aa9e86 · Cited by 10
Riedel, A. R., DiTomasso, V., Rice, E. L., Alam, M. K., Abrahams, E. S., Crook, J., Cruz, K. L., & Faherty, J. K. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab1915 · Cited by 9
The cosmic waltz of Coma Berenices and Latyshev 2 (Group X)
Olivares, J., Lodieu, N., Béjar, V. J. S., Martín, E. L., Žerjal, M., & Galli, P. A. B. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244703 · Cited by 9
A Lithium Depletion Age for the Carina Association
Wood, M. L., Mann, A. W., Barber, M. G., Bush, J. L., Milburn, R. P., Thao, P. C., Schmidt, S. P., Tofflemire, B. M., & Kraus, A. L. (2023) · The Astronomical Journal · doi:10.3847/1538-3881/ad03f3 · Cited by 9
“Tucana-Horologium may be independent from Carina-Columba (Kraus et al. 2014), or it may be part of the larger complex.”
BackgroundResultInfluentialSelf-citationSearching for new young stars in the Northern hemisphere: the Pisces moving group
Binks, A. S., Jeffries, R. D., & Ward, J. L. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx2252 · Cited by 9
“In this work we also include Li EW data for the β Pic MG (herein BPMG, age ∼ 20 − 25Myr, Binks & Jeffries 2014; Bell, Mamajek & Naylor 2015) compiled from the lists in Messina et al. (2016) and the Tucanae-Horologium MG (41 ± 2Myr, Kraus et al. 2014).”
MethodSpectral characterization of newly detected young substellar binaries with SINFONI
Calissendorff, P., Janson, M., Asensio-Torres, R., & Köhler, R. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201935319 · Cited by 9
“They both show strong signs of youth and share space velocities with the Argus YMG and ABD MG respectively, which in combination of assuming that all members of the YMGs are coeval can constrain their ages even further to 30 − 50 Myr for 2M1510 and 120 − 200 Myr for 2M2202.”
BackgroundInfluentialEvidence for Centrifugal Breakout around the Young M Dwarf TIC 234284556
Palumbo, E. K., Montet, B. T., Feinstein, A. D., Bouma, L. G., Hartman, J. D., Hillenbrand, L. A., Gully-Santiago, M., & Banks, K. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac38a5 · Cited by 9
“…are consistent with the Wα = −9.40 Å measured by Kraus et al. (2014) for this star, and broadly fit with the range of equivalent widths measured by Kraus et al. (2014) for young M dwarfs in the Tuc-Hor association and by Scholz et al. (2007) for M dwarfs in the slightly younger β Pictoris…”
BackgroundResultInfluentialToward Direct Imaging of Low-mass Gas-Giant Planets with the James Webb Space Telescope
Schlieder, J. E., Beichman, C. A., Meyer, M. R., & Greene, T. P. (2015) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921315006407 · Cited by 8
“For these reasons, many dedicated searches to identify the missing M dwarf members of YMGs have been undertaken, e.g. Kraus et al. (2014), and several surveys to directly image their planets are ongoing (Bowler et al. 2015).”
BackgroundTheissen, C., Burgasser, A., Gagliuffi, D. B. B., Hardegree-Ullman, K., Gagn'e, J., Schmidt, S. J., & West, A. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aaa0cf · Cited by 6
“The higher levels of MIR flux may be due to dust in the system, similar to what Boucher et al. (2016) discovered for 2MASSJ02265658 −5327032, an L0δ dwarf and possible member of the ∼40Myr Tucana–Horologium association (Kraus et al. 2014).”
BackgroundA Radial velocity survey of spatially resolved young, low-mass binaries
Durkan, S., Janson, M., Ciceri, S., Brandner, W., Schlieder, J. E., Henning, T. K., Bonnefoy, M., Kankare, J., & Watson, C. A. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201732156 · Cited by 8
“In our previous AstraLux M-dwarf multiplicity studies, targets were selected from multiple catalogs of late type stars on the basis of youth; indicated by high-probability YMG membership (e.g., Malo et al. 2013, 2014; Kraus et al. 2014) and X-ray emission (Lépine & Gaidos 2011).”
MethodJackman, J. A. G., Shkolnik, E. L., Loyd, R. O. P., & Richey-Yowell, T. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1570 · Cited by 7
Self-citationTofflemire, B. M., Kraus, A. L., Mann, A. W., Newton, E. R., Gully-Santiago, M., Vanderburg, A. M., Waalkes, W. C., Berta-Thompson, Z. K., Collins, K. I., Collins, K. A., et al. (2023) · The Astronomical Journal · doi:10.3847/1538-3881/aca60f · Cited by 7
“Our search recovers many bona fide members of the Columba association, whose CMD distribution is consistent with the 40Myr Tuc–Hor sequence.”
BackgroundMethodInfluentialSelf-citationCan scallop-shell stars trap dust in their magnetic fields?
Sanderson, H., Jardine, M., Cameron, A. C., Morin, J., & Donati, J. ‐. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3302 · Cited by 7
Kerr, R. M. P., Kraus, A. L., Krolikowski, D. M., Bouma, L. G., & Farias, J. P. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad7135 · Cited by 7
“This pattern has been seen in other young populations, and is likely caused by slight model inaccuracies in the evolution of stars in this section of the pre-main sequence (Kraus et al. 2014).”
BackgroundSelf-citationThe Isochronal Age Scale of Young Moving Groups in the Solar Neighbourhood
Bell, C. P. M., Mamajek, E. E., & Naylor, T. (2015) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921315006213 · Cited by 5
“…are advocated in the recent review of young stellar ages by Soderblom et al. (2014) to provide our best chance of establishing a reliable and robust age scale in the range 20− 200Myr, have been demonstrated to be systematically older when compared to isochronal ages (see e.g. Kraus et al. 2014).”
BackgroundAguirre, F. C., Youngblood, A. A., France, K. C., & Bourrier, V. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acad7d · Cited by 5
“(1) Keenan & McNeil (1989), (2) Nidever et al. (2002), (3) Gaia Collaboration (2018), (4) Soubiran et al. (2018), (5) Torres et al. (2006), (6) Kraus et al. (2014), (7) Riedel et al. (2017), (8) Riaz et al. (2006), (9) Endl et al. (2006), (10) Gray et al. (2003), (11) Stephenson (1986), (12) Chubak…”
Characterization of close visual binaries from the AstraLux Large M Dwarf Survey
Bergfors, C., Brandner, W., Bonnefoy, M., Schlieder, J. E., Janson, M., Henning, T. K., & Chauvin, G. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2768 · Cited by 5
“The EW of Li in J024902 A is weaker than in M1−M2 type members of the ≈ 10Myr TW Hydrae association, but stronger than members of the ≈ 40 Myr old Tucana-Horologium association (Kraus et al. 2014).”
BackgroundExoplaNeT accRetion mOnitoring sPectroscopic surveY (ENTROPY)
Demars, D., Bonnefoy, M., Dougados, C., Viswanath, G., Ringqvist, S. C., Janson, M., Aoyama, Y., Thanathibodee, T., Marleau, G.-D., Manara, C. F., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202554644 · Cited by 4
The planetary-mass-limit VLT/SINFONI library
Palma-Bifani, P., Bonnefoy, M., Chauvin, G., Rojo, P., Baudoz, P., Charnay, B., Denis, A., Hoch, K. K. W., Petrus, S., Ravet, M., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202554894 · Cited by 4
A GALEX Far-ultraviolet Study of Dwarf Stars in Moving Groups
Cochrane, K. M., & Smith, G. H. (2019) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/ab3712 · Cited by 4
Tofflemire, B. M., Rizzuto, A. C., Newton, E. R., Kraus, A. L., Mann, A. W., Vanderburg, A. M., Nelson, T., Hawkins, K., Wood, M. L., Zhou, G., et al. (2021) · DSpace@MIT (Massachusetts Institute of Technology) · Cited by 4
Self-citationBattley, M. P., Armstrong, D. J., & Pollacco, D. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac278 · Cited by 4
Pleiades or Not? Resolving the Status of the Lithium-rich M Dwarfs HHJ 339 and HHJ 430
Stauffer, J., Barrado, D., David, T. J., Rebull, L. M., Hillenbrand, L. A., Mamajek, E. E., Oppenheimer, R., Aigrain, S., Bouy, H., & Lillo-Box, J. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/ab93c9 · Cited by 4
Companion mass limits for 17 binary systems obtained with binary differential imaging and MagAO/Clio
Pearce, L., Males, J. R., Weinberger, A. J., Long, J. D., Morzinski, K. M., Close, L. M., & Hinz, P. M. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2056 · Cited by 4
Anomalous Spectral Types and Intrinsic Colors of Young Stars
Pecaut, M. J. (2015) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921315006079 · Cited by 4
Lost Sisters Found: TESS and Gaia Reveal a Dissolving Pleiades Complex
Boyle, A. W., Bouma, L. G., & Mann, A. W. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ae0724 · Cited by 3
“As an example, some cooler stars from Chameleon ( t ≲ 17 Myr; R. Kerr et al. 2023) and Tuc-Hor ( t ≈ 40 Myr; A. L. Kraus et al. 2014) appear in our membership list due to this blurring of the rotation sequence at young ages.”
James, D. J., Aarnio, A., Richert, A. J. W., Cargile, P. A., Santos, N. C., Melo, C., & Bouvier, J. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw481 · Cited by 3
“9-7901 appear to be considerably older than the 5-10 Myr age of the group (Lawson et al. 2001, Luhman & Steeghs 2004), having ages at least 25-30 Myr, more appropriate to those of post T-Tauri stars.”
BackgroundMethodInfluentialFlare frequency in M dwarfs belonging to young moving groups
Mamonova, E., Shan, Y., Kowalski, A. F., Wedemeyer, S., & Werner, S. C. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202554614 · Cited by 3
Planet interactions at a young age
Micela, G., Cecchi-Pestellini, C., Colombo, S., Locci, D., & Petralia, A. (2021) · Astronomische Nachrichten · doi:10.1002/asna.20210097 · Cited by 3
Fields, M. J., Mann, A. W., Kesseli, A. Y., & Boyle, A. W. (2025) · RAS Techniques and Instruments · doi:10.1093/rasti/rzaf009 · Cited by 3
Phillips, C. L., Bowler, B. P., Mace, G., Liu, M. C., & Sokal, K. R. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab9111 · Cited by 4
Self-citationSPYGLASS. VII-A. The Demographics and Ages of Small Nearby Young Associations
Kerr, R. M. P., Paolino, F. P., Tan, J. C., Speagle, J. S., Kraus, A. L., Fernández-Trincado, J. G., Stassun, K. G., & Chanamé, J. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ae1731 · Cited by 2
“Following Kraus et al. (2014), we mark stars below this empirical limit as H α non-members, unless they show evidence for unresolved bi-narity ( RUWE > 1 .”
Self-citationKinematic Ages of the Tucana–Horologium, Columba, and Carina Associations
Couture, D., Gagné, J., & Doyon, R. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae1d79 · Cited by 2
“…± 4 Myr ( C. P. M. Bell et al. 2015 ) , 21 ± 4 Myr ( L. Malo et al. 2014b ) , and 30 Myr ( C. A. O. Torres et al. 2000 ) , and the LDB method, 40 ± 3 Myr ( A. L. Kraus et al. 2014 ) , 27 ± 11 Myr ( E. Mentuch et al. 2008 ) , and, more recently, + 51.0 0.20.5 Myr ( F. J. Galindo-Guil et al. 2022 ) .”
InfluentialRamírez-Preciado, V., Román-Zúñiga, C. G., Aguilar, L. A., Suárez, G., & Downes, J. J. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aae202 · Cited by 2
ACRONYM IV: Three New, Young, Low-mass Spectroscopic Binaries
Flagg, L., Shkolnik, E. L., Weinberger, A. J., Bowler, B. P., Skiff, B. A., Kraus, A. L., & Liu, M. C. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab9083 · Cited by 2
“Thus far, the program has classified 129 new low-mass members of the 40Myr Tuc-Hor Moving Group (Kraus et al. 2014), 41 new low-mass members of the 23Myr Beta Pic Moving Group (Shkolnik et al. 2017), and 77 members of other groups (Schneider et al. 2019).”
BackgroundMethodInfluentialSelf-citationA Search for Stellar Siblings of the ∼200 Myr TOI-251 b Planetary System
Sun, Q., Wang, S. X., Mann, A. W., Tofflemire, B. M., Kraus, A. L., Gan, T., & Barber, M. G. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acd346 · Cited by 3
“The candidate stars show a clearly defined main-sequence that falls in between the Tuc-Hor (Kraus et al. 2014) young association and the Mamajek sequence (typical main sequence for the Solar Neighborhood, Pecaut & Mamajek 2013).”
BackgroundResultSelf-citationWalkaway Star Candidates in IC 348 and Their Possible Birthplaces
Zhou, X., Herczeg, G. J., Fang, M., Wang, X.-L., & Ren, B. B. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/aced86 · Cited by 2
Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Bogat, E., Schlieder, J. E., Lawson, K., Li, Y., Leisenring, J., Meyer, M. R., Balmer, W. O., Barclay, T., Beichman, C., Bryden, G., et al. (2025) · The Astronomical Journal · doi:10.3847/1538-3881/adfc75 · Cited by 2
“…than a decade to identify all late K and M dwarf stars confirmed or proposed as members of young moving groups and associations and compile a candidate list ( e.g., B. Zuckerman & I. Song 2004; C. A. O. Torres et al. 2008; E. L. Shkolnik et al. 2012; A. L. Kraus et al. 2014; L. Malo et al. 2014 ) .”
Brown Dwarfs and Free-Floating Planets in Young Stellar Clusters
Béjar, V. J. S., & Martín, E. L. (2018) · Springer eBooks · doi:10.1007/978-3-319-30648-3_92-1 · Cited by 2
Multifilter observations of the complex periodic variations in eight pre-main sequence stars
Koen, C. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3276 · Cited by 2
Popinchalk, M., Faherty, J. K., Gagné, J., Curtis, J. L., Moranta, L., Kiman, R., Couture, D., Jusino, A., Paliwal, G., Mouzakitis, I., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad5b56 · Cited by 1
THYME. XIII. Two Young Neptunes Orbiting a 75 Myr Star in the Alpha Persei Cluster
Dattilo, A., Vanderburg, A. M., Barber, M. G., Mann, A. W., Kerr, R. M. P., Kraus, A. L., Livesey, J. R., Watkins, C. N., Collins, K. A., García‐Mejía, J., et al. (2025) · The Astronomical Journal · doi:10.3847/1538-3881/ae0a35 · Cited by 1
Self-citationThe SPHERE infrared survey for exoplanets (SHINE)
Squicciarini, V., Desidera, S., Chauvin, G., Kiefer, F., D’Orazi, V., Fontanive, C., Vigan, A., Nardiello, D., Messina, S., Albert, D., et al. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202658983 · Cited by 1
SPYGLASS. VII-B. Tracing the Fragments of Massive Star Formation Using Low-mass Associations
Kerr, R. M. P., Kraus, A. L., Tan, J. C., Chanamé, J., Paolino, F. P., Speagle, J. S., Farias, J. P., Fernández-Trincado, J. G., & Hawkins, K. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae665e · Cited by 1
“The oldest populations in the Local Family are IC 2602 and Tuc-Hor, which have similar ages of ∼ 45 Myr (A. L. Kraus et al. 2014; S. Randich et al. 2018; M. L. Wood et al. 2023).”
Self-citationLithium Depletion Boundary Ages of Young Stars: Inconsistencies in Pre-Main Sequence Models
Song, I. (2015) · Proceedings of the International Astronomical Union · doi:10.1017/s174392131500664x · Cited by 1
“In this paper, an SED-fitting approach is used instead and, because of the covariance nature of several photometric magnitudes for a given source, this method is known to be very robust (Kraus et al. 2014).”
MethodLiu, M. C., Magnier, E. A., Zhang, Z., Gaidos, E. J., Dupuy, T. J., Liu, P., Biller, B. A., Vos, J. M., Allers, K., Hinkle, J. T., et al. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac8cee · Cited by 1
“Substantial disks older than ∼20 Myr are rare (e.g., Kraus et al. 2014 find a frequency of <0.8% for optically thick and thin disks around M dwarfs in the ∼40 Myr old Tuc-Hor Association), but they do exist.”
BackgroundMethodInfluentialSelf-citationNearby Young Stars and Young Moving Groups
Kastner, J. H., & Principe, D. A. (2022) · Springer eBooks · doi:10.1007/978-981-16-4544-0_83-1 · Cited by 1
Mizuki, T., Kuzuhara, M., Mede, K., Schlieder, J. E., Janson, M., Brandt, T. D., Hirano, T., Narita, N., Wisniewski, J. P., Yamada, T., et al. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aada82 · Cited by 1
“…young stars including candidates and their observed properties from the literature (Ansdell et al. 2015; da Silva et al. 2009; Frasca et al. 2015; Kraus et al. 2014; Meibom et al. 2009, 2011; Messina et al. 2017; Newton et al. 2017; Rebull et al. 2016; Schneider et al. 2012, and references…”
BackgroundBrown Dwarfs and Free-Floating Planets in Young Stellar Clusters
Béjar, V. J. S., & Martín, E. L. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_92 · Cited by 1
Nearby Young Stars and Young Moving Groups
Kastner, J. H., & Principe, D. A. (2024) · Springer eBooks · doi:10.1007/978-981-19-6960-7_83
Brown Dwarfs and Free-Floating Planets in Young Stellar Clusters
Béjar, V. J. S., & Martín, E. L. (2025) · Springer eBooks · doi:10.1007/978-3-319-30648-3_92-2
The stellar initial mass function of nearby young moving groups
Bertolotto-Stefanelli, R., Downes, J. J., Suárez, G., Mateu, C., Gagné, J., & Zúñiga, C. R. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202557920
Observational constraints on the chemical tracers of planet formation history
Hayoz, J., Bonse, M. J., Garvin, E. O., Cugno, G., Dannert, F., Kühnle, H., Rosa, R. J. D., Berbel, A. A., Cao, Y., de Xivry, G. O., et al. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202557546
Metadata
- Authors
- Kraus, A. L., Shkolnik, E. L., Allers, K. N., & Liu, M. C.
- Affiliations
- Center for Astrophysics Harvard & Smithsonian (US)
- Lowell Observatory (US)
- Bucknell University (US)
- University of Hawaiʻi at Mānoa (US)
- Venue
- The Astronomical Journal
- Publisher
- American Astronomical Society
- Published
- 2014-05-08
- Volume
- 147
- Issue
- 6
- Pages
- 146
- ISSN
- 0004-6256 (ISSN-L)
- 1538-3881
- OpenAlex
- W1979315153
- Cited by
- 199
- References
- 84
- Citations by year
- 2026: 5 · 2025: 10 · 2024: 8 · 2023: 16 · 2022: 22 · 2021: 13 · 2020: 19 · 2019: 21 · 2018: 20 · 2017: 14 · 2016: 21 · 2015: 20 · 2014: 10
- FWCI
- 11.68
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Licence
- Locations
- The Astronomical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Keywords
- young stellar populations, K and M dwarfs, lithium depletion, lithium depletion boundary, H-alpha emission, radial velocity, kinematic selection, debris disks, X-ray activity, ROSAT, isochronal ages, pre-main-sequence stars
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