The DOI matches its Crossref record; 84 of the 84 references it cites were found in a registry or an index.
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
Cites
The Two Micron All Sky Survey (2MASS)
Skrutskie, M. F., Cutri, R. M., Stiening, R., Weinberg, M. D., Schneider, S., Carpenter, J. M., Beichman, C., Capps, R., Chester, T., Elias, J., et al. (2006) · The Astronomical Journal · doi:10.1086/498708 · Cited by 12,019 · cited 1×
“2MASS The Two-Micron All-Sky Survey (2MASS; Skrutskie et al. 2006) observed the entire sky in the J, H, and Ks bands over the interval of 1998–2002.”
MethodGalactic Stellar and Substellar Initial Mass Function
Chabrier, G. (2003) · Publications of the Astronomical Society of the Pacific · doi:10.1086/376392 · Cited by 9,071 · cited 4×
“Tuc-Hor is likely one of the largest young stellar populations within d 100 pc, making it a robust site for measuring population statistics (the IMF, multiplicity properties, disk frequencies, and activity rates).”
BackgroundInfluentialThe Sloan Digital Sky Survey: Technical Summary
York, D., Adelman, J., Anderson, J., Anderson, S., Annis, J., Bahcall, N., Bakken, J., Barkhouser, R., Bastian, S., Berman, E., et al. (2000) · The Astronomical Journal · doi:10.1086/301513 · Cited by 8,368 · cited 1×
“SDSS The Sloan Digital Sky Survey (SDSS; York et al. 2000) is an ongoing deep optical imaging and spectroscopic survey of the northern galactic cap and selected regions of the southern cap.”
BackgroundThe Luminosity function and stellar evolution
Salpeter, E. (1955) · The Astrophysical Journal · doi:10.1086/145971 · Cited by 6,816 · cited 4×
“Tuc-Hor is likely one of the largest young stellar populations within d 100 pc, making it a robust site for measuring population statistics (the IMF, multiplicity properties, disk frequencies, and activity rates).”
BackgroundInfluentialTurbulence and star formation in molecular clouds
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The Galaxy Evolution Explorer : A Space Ultraviolet Survey Mission
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“…the higher completeness of using UV wavelengths to search for young M dwarfs (Findeisen & Hillenbrand 2010; Shkolnik et al. 2011; Rodriguez et al. 2011, 2013), making the NASA Galaxy Evolution Explorer (GALEX; Martin et al. 2005) a useful resource with which to expand the young low-mass census.”
BackgroundINTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS
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×
“The dwarf and young-star temperature scales of Pecaut & Mamajek (2013) both fall between these limits.”
BackgroundMonet, D. G., Levine, S. E., Canzian, B., Ables, H. D., Bird, A. R., Dahn, C. C., Guetter, H. H., Harris, H. C., Henden, A. A., Leggett, S. K., et al. (2003) · The Astronomical Journal · doi:10.1086/345888 · Cited by 2,203
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×
“Given a short-period binary frequency of F ∼ 10% for a < 2 AU (e.g., Raghavan et al. 2010), then our 142 members should be matched by ∼14 SBs that could have been rejected by their discrepant RVs, much as the 34 objects confirmed by Li include 5 RVdiscrepant objects that likely are SB1s.”
BackgroundDirect Imaging of Multiple Planets Orbiting the Star HR 8799
Marois, C., Macintosh, B., Barman, T., Zuckerman, B., Song, I., Patience, J. L., Lafreniére, D., & Doyon, R. (2008) · Science · doi:10.1126/science.1166585 · Cited by 1,711 · cited 1×
“…these young moving groups makes them especially advantageous for the study of circumstellar processes that depend on angular resolution (such as multiple star formation; Brandeker et al. 2003, 2006; Evans et al. 2012) and searches for extrasolar planets (Marois et al. 2008; Lagrange et al. 2009).”
Background
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Cited by
Sorted by citations
Gagné, J., Mamajek, E. E., Malo, L., Riedel, A. R., Rodriguez, D., Lafreniére, D., Faherty, J. K., Roy-Loubier, O., Pueyo, L. A., Robin, A. C., et al. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaae09 · Cited by 565
“…et al. 2001; (35) Neuhäuser et al. 2003; (36) Zuckerman & Song 2004; (37) Gontcharov 2006; (38) Anderson & Francis 2012; (39) Bobylev et al. 2006; (40) Kraus et al. 2014; (41) Zuckerman & Webb 2000; (42) Grenier et al. 1999; (43) Pecaut & Mamajek 2013; (44) Elliott et al. 2014; (45) Webb et…”
BackgroundMethodResultInfluentialA self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood
Bell, C. P. M., Mamajek, E. E., & Naylor, T. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1981 · Cited by 509
“Not accounting for unresolved multiples, our sample includes a total of 89 members of the AB Dor moving group, 27 members of Argus, 97 members of the BPMG, 12 members of Carina, 50 members of Columba, 18 members of η Cha, 189 members of Tuc-Hor, 30 members of TWA, and 14 members of 32 Ori.”
BackgroundMethodResultInfluentialImaging Extrasolar Giant Planets
Bowler, B. P. (2016) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/128/968/102001 · Cited by 450
“Several planetary-mass companions have been imaged around binary stars on wide circumbinary orbits: ROXs 42B b (Kraus et al. 2014a; Currie et al. 2014b), Ross 458 c (Goldman et al. 2010; Scholz 2010), SR 12 C (Kuzuhara et al. 2011), HD 106906 b (Bailey et al. 2014; Lagrange et al. 2016), and VHS…”
BackgroundInfluentialMann, A. W., Dupuy, T., Kraus, A. L., Gaidos, E. J., Ansdell, M., Ireland, M., Rizzuto, A. C., Hung, C.-L., Dittmann, J., Factor, S. M., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaf3bc · Cited by 367
Self-citationKraus, A., Ireland, M., Huber, D., Mann, A., & Dupuy, T. (2016) · The Astronomical Journal · doi:10.3847/0004-6256/152/1/8 · Cited by 232
“0 (Monet et al. 2003), as described in Kraus & Hillenbrand (2007) and Kraus et al. (2014), to estimate both parameters.”
BackgroundSelf-citation
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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