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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Cites
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“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 Luminosity function and stellar evolution
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BackgroundInfluentialTurbulence and star formation in molecular clouds
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BackgroundINTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS
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A SURVEY OF STELLAR FAMILIES: MULTIPLICITY OF SOLAR-TYPE STARS
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“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× · see citing works
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BackgroundAstrometric Calibration of the Sloan Digital Sky Survey
Pier, J. R., Munn, J. A., Hindsley, R. B., Hennessy, G. S., Kent, S. M., Lupton, R. H., & Ivezić, Ž. (2003) · The Astronomical Journal · doi:10.1086/346138 · Cited by 908 · cited 1× · see citing works
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MethodA Universal Stellar Initial Mass Function? A critical look at variations in extreme environments
Bastian, N., Covey, K., & Meyer, M. (2010) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-082708-101642 · Cited by 812 · cited 1× · see citing works
“Given the strong evidence that the IMF is universal for most young populations in the solar neighborhood (e.g., Bastian et al. 2010 and references therein), then a comparison of Tuc-Hor to the standard IMF can demonstrate which mass ranges of members are still incomplete.”
BackgroundRoêser, S., Demleitner, M., & Schilbach, E. (2010) · The Astronomical Journal · doi:10.1088/0004-6256/139/6/2440 · Cited by 781 · see citing works
Optimal Techniques in Two‐dimensional Spectroscopy: Background Subtraction for the 21st Century
Kelson, D. D. (2003) · Publications of the Astronomical Society of the Pacific · doi:10.1086/375502 · Cited by 685 · cited 1× · see citing works
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MethodRadial Velocities for 889 Late‐Type Stars
Nidever, D. L., Marcy, G. W., Butler, R. P., Fischer, D. A., & Vogt, S. S. (2002) · The Astrophysical Journal Supplement Series · doi:10.1086/340570 · Cited by 679 · cited 2× · see citing works
“We also observed standard stars nightly from the list of Nidever et al. (2002), which serve as both RV and spectral type templates, as well as most of the known Tuc-Hor members with SpT≥K3, numerous members of the ScoCen OB association, and a selection of known members from other nearby young…”
BackgroundMethodZuckerman, B., & Song, I. (2004) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.42.053102.134111 · Cited by 593 · cited 6× · see citing works
“100 Myr) have been identified among the nearby field population (Kastner et al. 1997; Webb et al. 1999; Mamajek et al. 1999; Torres et al. 2000; Zuckerman & Webb 2000; Zuckerman & Song 2004).”
BackgroundMethodInfluentialA Census of the Young Cluster IC 348
Luhman, K. L., Stauffer, J. R., Muench, A. A., Rieke, G. H., Lada, E. A., Bouvier, J., & Lada, C. J. (2003) · The Astrophysical Journal · doi:10.1086/376594 · Cited by 589 · cited 1× · see citing works
“If we use the young-star temperature sequence of Luhman et al. (2003) for ≥M1, the sequence is shifted ∼0.5 subclass later for a given mass or temperature.”
MethodInfluentialA probable giant planet imaged in the β Pictoris disk
Lagrange, A. ‐., Gratadour, ., Chauvin, G., Fusco, T., Ehrenreich, D., Mouillet, D., Rousset, G., Rouan, D., Allard, F. C., Gendron, E., et al. (2008) · Astronomy and Astrophysics · doi:10.1051/0004-6361:200811325 · Cited by 570 · see citing works
Pecaut, M. J., Mamajek, E. E., & Bubar, E. J. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/746/2/154 · Cited by 564 · cited 1× · see citing works
“This trend is consistent with the results of Pecaut et al. (2012), who use several other age diagnostics to determine that the Upper Scorpius subgroup of the Sco-Cen OB association might be a factor of ∼2 older (τ ∼ 11 Myr) than its traditionally accepted isochronal age for low-mass members (τ ∼ 5…”
ResultThe Origin of T Tauri X‐Ray Emission: New Insights from the Chandra Orion Ultradeep Project
Preibisch, T., Kim, Y., Favata, F., Feigelson, E. D., Flaccomio, E., Getman, K. V., Micela, G., Sciortino, S., Stassun, K. G., Stelzer, B., et al. (2005) · The Astrophysical Journal Supplement Series · doi:10.1086/432891 · Cited by 529 · cited 2× · see citing works
“Selection of Young Stars with GALEX Stellar activity is known to be an indicator of youth (Preibisch et al. 2002, 2005), so X-ray and UV all-sky surveys are well-suited to finding active young stars.”
BackgroundL′ andM′ Photometry of Ultracool Dwarfs
Golimowski, D. A., Leggett, S. K., Marley, M. S., Fan, X., Geballe, T. R., Knapp, G. R., Vrba, F. J., Henden, A. A., Luginbuhl, C. B., Guetter, H. H., et al. (2004) · The Astronomical Journal · doi:10.1086/420709 · Cited by 486 · cited 1× · see citing works
“We converted the model Teff values to spectral types using the dwarf temperature sequence of Schmidt-Kaler (1982) for ≤M0 stars and the dwarf sequence of Golimowski et al. (2004) for ≥M1 stars.”
MethodStauffer, J. R., Schultz, G. V., & Kirkpatrick, J. D. (1998) · The Astrophysical Journal · doi:10.1086/311379 · Cited by 456 · cited 3× · see citing works
“50 pc) have subsequently identified several additional populations, including the AB Dor, Carina-Near, HerculesLyra, and Tucana-Horologium associations (Zuckerman & Song 2004; Zuckerman et al. 2006; Torres et al. 2008; Eisenbeiss et al. 2013).”
BackgroundResultInfluentialDiscovery of Seven T Tauri Stars and a Brown Dwarf Candidatein the Nearby TW Hydrae Association
Webb, R. A., Zuckerman, B., Platais, I., Patience, J., White, R. J., Schwartz, M. J., & McCarthy, C. (1999) · The Astrophysical Journal · doi:10.1086/311856 · Cited by 396 · cited 1× · see citing works
“100 Myr) have been identified among the nearby field population (Kastner et al. 1997; Webb et al. 1999; Mamajek et al. 1999; Torres et al. 2000; Zuckerman & Webb 2000; Zuckerman & Song 2004).”
BackgroundX-ray and Molecular Emission from the Nearest Region of Recent Star Formation
Kastner, J. H., Zuckerman, B., Weintraub, D. A., & Forveille, T. (1997) · Science · doi:10.1126/science.277.5322.67 · Cited by 385 · cited 1× · see citing works
“100 Myr) have been identified among the nearby field population (Kastner et al. 1997; Webb et al. 1999; Mamajek et al. 1999; Torres et al. 2000; Zuckerman & Webb 2000; Zuckerman & Song 2004).”
BackgroundThe On-Orbit Performance of the Galaxy Evolution Explorer
Morrissey, P. F., Schiminovich, D., Barlow, T. A., Martin, D. C., Blakkolb, B. K., Conrow, T., Cooke, B., Erickson, K. D., Fanson, J. L., Friedman, P. G., et al. (2005) · The Astrophysical Journal · doi:10.1086/424734 · Cited by 364 · cited 2× · see citing works
“The full description of the instrumental performance is presented by Morrissey et al. (2005).”
BackgroundMethodInfluentialBAYESIAN ANALYSIS TO IDENTIFY NEW STAR CANDIDATES IN NEARBY YOUNG STELLAR KINEMATIC GROUPS
Malo, L., Doyon, R., Lafreniére, D., Artigau, É., Gagné, J., Baron, F., & Riedel, A. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/762/2/88 · Cited by 361 · see citing works
Exploring the Full Stellar Population of the Upper Scorpius OB Association
Preibisch, T., Brown, A. G. A., Bridges, T. J., Guenther, E. W., & Zinnecker, H. (2002) · The Astronomical Journal · doi:10.1086/341174 · Cited by 349 · cited 3× · see citing works
“Selection of Young Stars with GALEX Stellar activity is known to be an indicator of youth (Preibisch et al. 2002, 2005), so X-ray and UV all-sky surveys are well-suited to finding active young stars.”
BackgroundAn Assessment of Dynamical Mass Constraints on Pre–Main‐Sequence Evolutionary Tracks
Hillenbrand, L. A., & White, R. J. (2004) · The Astrophysical Journal · doi:10.1086/382021 · Cited by 319 · cited 1× · see citing works
“These system velocities are more uncertain due to the significant systematic uncertainties in pre-main sequence evolutionary models (e.g., Hillenbrand & White 2004), but based on the members which can be independently confirmed from lithium or Hα (and hence should be comoving with Tuc-Hor), we…”
BackgroundThe Stellar Populations of Praesepe and Coma Berenices
Kraus, A. L., & Hillenbrand, L. A. (2007) · The Astronomical Journal · doi:10.1086/522831 · Cited by 316 · cited 8× · see citing works
“We describe the motivation and details in Kraus & Hillenbrand (2007).”
BackgroundMethodInfluentialSelf-citationTHE SLOAN DIGITAL SKY SURVEY DATA RELEASE 7 SPECTROSCOPIC M DWARF CATALOG. I. DATA
West, A. A., Morgan, D. P., Bochanski, J. J., Andersen, J. M., Bell, K. J., Kowalski, A. F., Davenport, J. R. A., Hawley, S. L., Schmidt, S. J., Bernat, D., et al. (2011) · The Astronomical Journal · doi:10.1088/0004-6256/141/3/97 · Cited by 311 · cited 2× · see citing works
“• Hα emission: Old main sequence stars exhibit a wide range of activity levels (e.g., Kafka & Honeycutt 2006; West et al. 2011), and hence the presence of strong Hα emission can not be used as a positive criterion for determining membership.”
BackgroundSearch for Associations Containing Young stars (SACY): I. Sample & Searching MethodPreprint
Torres, C. A. O., Quast, G. R., da Silva, L., Reza, R. D. L., Melo, C., & Sterzik, M. (2006) · arXiv (Cornell University) · doi:10.1051/0004-6361:20065602 · Cited by 309 · cited 3× · see citing works
“The SACY search of Tuc-Hor (Torres et al. 2006, 2008) found 17 members with spectral types of K3-M0, of which we recovered 15 as candidates.”
BackgroundResultInfluentialZuckerman, B., Rhee, J. H., Song, I., & Bessell, M. S. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/732/2/61 · Cited by 275 · cited 1× · see citing works
“Most programs have only identified a small number of candidates (Kiss et al. 2011) or have concentrated on higher-mass membership (Zuckerman & Song 2004; Torres et al. 2006, 2008; Zuckerman et al. 2011).”
BackgroundBrown Dwarfs and the TW Hydrae Association
Gizis, J. E. (2002) · The Astrophysical Journal · doi:10.1086/341259 · Cited by 253 · cited 1× · see citing works
“The low distances also result in additional sensitivity for flux-limited studies of disks (Low et al. 2005; Bouwman et al. 2006; Plavchan et al. 2009) and the (sub)stellar mass function (Gizis 2002; Lyo et al. 2006; Murphy et al. 2010; Shkolnik et al. 2011).”
BackgroundTHE DISK POPULATION OF THE UPPER SCORPIUS ASSOCIATION
Luhman, K. L., & Mamajek, E. E. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/758/1/31 · Cited by 235 · cited 1× · see citing works
“Based on the criteria suggested by Luhman & Mamajek (2012), all targets are Class III (diskless) sources with W1 − W3 1.”
MethodSpectroscopy of Very Low Mass Stars and Brown Dwarfs in IC 2391: Lithium Depletion and Hα Emission
Barrado, D., Stauffer, J. R., & Jayawardhana, R. (2004) · The Astrophysical Journal · doi:10.1086/423485 · Cited by 234 · cited 1× · see citing works
“Barrado y Navascués et al. (2004) reported a boundary at Mbol = 10.24± 0.15 in IC 2391, as well as updating the results of Stauffer et al. (1998, 1999) for α Per (Mbol = 11.31 ± 0.15) and the Pleiades (Mbol = 12.14 ± 0.15).”
ResultInfluentialA lithium depletion boundary age of 21 Myr for the Beta Pictoris moving group
Binks, A. S., & Jeffries, R. D. (2013) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slt141 · Cited by 234 · see citing works
A Moving Cluster Distance to the Exoplanet 2M1207b in the TW Hydrae Association
Mamajek, E. E. (2005) · The Astrophysical Journal · doi:10.1086/468181 · Cited by 232 · cited 1× · see citing works
“• Radial velocities: By definition, young moving groups are comoving with a very small velocity dispersion (σ ∼1 km/s for TWA; Mamajek 2005), and hence the radial velocities of Tuc-Hor members should correlate very well with the projection of the group UVW velocity into the line of sight.”
BackgroundIdentification of New M Dwarfs in the Solar Neighborhood
Riaz, B., Gizis, J. E., & Harvin, J. A. (2006) · The Astronomical Journal · doi:10.1086/505632 · Cited by 223 · cited 2× · see citing works
“Most of our new members are not found in the active M dwarf census of Riaz et al. (2006), and indeed, the majority do not have ROSAT counterparts at all; only 53 of our 129 previously unidentified members have an X-ray counterpart in the ROSAT All-Sky Survey within <30′′.”
BackgroundNEW DEBRIS DISKS AROUND YOUNG, LOW-MASS STARS DISCOVERED WITH THESPITZER SPACE TELESCOPE
Plavchan, P., Werner, M. W., Chen, C. H., Stapelfeldt, K. R., Su, K. Y. L., Stauffer, J. R., & Song, I. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/698/2/1068 · Cited by 209 · cited 1× · see citing works
“The low distances also result in additional sensitivity for flux-limited studies of disks (Low et al. 2005; Bouwman et al. 2006; Plavchan et al. 2009) and the (sub)stellar mass function (Gizis 2002; Lyo et al. 2006; Murphy et al. 2010; Shkolnik et al. 2011).”
BackgroundTHE MASS-RADIUS(-ROTATION?) RELATION FOR LOW-MASS STARS
Kraus, A. L., Tucker, R. A., Thompson, M. I., Craine, E. R., & Hillenbrand, L. A. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/728/1/48 · Cited by 207 · cited 1× · see citing works
“This process is described in more detail in Kraus et al. (2011) and Law 8 http://www.astro.utoronto.ca/ rucinski/ 8 et al. (2012).”
MethodSelf-citationIDENTIFYING THE YOUNG LOW-MASS STARS WITHIN 25 PC. I. SPECTROSCOPIC OBSERVATIONS
Shkolnik, E., Liu, M. C., & Reid, I. N. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/699/1/649 · Cited by 205 · cited 9× · see citing works
“We ultimately trace this paucity of identified candidates to their choice of input samples, which were based on ROSAT or GALEX.”
BackgroundInfluentialSelf-citationStauffer, J. R., Hartmann, L. W., Prosser, C. F., Randich, S., Balachandran, S., Patten, B. M., Simon, T., & Giampapa, M. S. (1997) · The Astrophysical Journal · doi:10.1086/303930 · Cited by 204 · cited 1× · see citing works
“However, young stars exhibit a lower bound on their Hα emission as a function of spectral type, and this boundary has been well-determined for the similaraged clusters IC 2602 and IC 2391 (Stauffer et al. 1997).”
BackgroundThe η Chamaeleontis Cluster: A Remarkable New Nearby Young Open Cluster
Mamajek, E. E., Lawson, W. A., & Feigelson, E. D. (1999) · The Astrophysical Journal · doi:10.1086/312005 · Cited by 181 · cited 1× · see citing works
“100 Myr) have been identified among the nearby field population (Kastner et al. 1997; Webb et al. 1999; Mamajek et al. 1999; Torres et al. 2000; Zuckerman & Webb 2000; Zuckerman & Song 2004).”
BackgroundMeeting the Cool Neighbors. VIII. A Preliminary 20 Parsec Census from the NLTT Catalogue
Reid, I. N., Cruz, K. L., Allen, P., Mungall, F., Kilkenny, D., Liebert, J., Hawley, S. L., Fraser, O. J., Covey, K. R., Lowrance, P., et al. (2004) · The Astronomical Journal · doi:10.1086/421374 · Cited by 180 · cited 1× · see citing works
“…be robustly calibrated for the age of Tuc-Hor, then their measurement for stars unaffiliated with any moving group can distinguish analogs to stars in star-forming regions (τ = 1–20 Myr) from the young (τ = 50–300 Myr) field population (Shkolnik et al. 2012) and old field stars (Reid et al. 2004).”
IDENTIFYING THE YOUNG LOW-MASS STARS WITHIN 25 pc. II. DISTANCES, KINEMATICS, AND GROUP MEMBERSHIP
Shkolnik, E. L., Anglada-Escudé, G., Liu, M. C., Bowler, B. P., Weinberger, A. J., Boss, A. P., Reid, I. N., & Tamura, M. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/758/1/56 · Cited by 175 · cited 10× · see citing works
“We ultimately trace this paucity of identified candidates to their choice of input samples, which were based on ROSAT or GALEX.”
BackgroundInfluentialSelf-citationSearch for associations containing young stars (SACY)
da Silva, L., Torres, C. A. O., Reza, R. D. L., Quast, G. R., Melo, C., & Sterzik, M. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200911736 · Cited by 164 · cited 1× · see citing works
“However, our census only adds a modest number of stars with SpT earlier than K5, so we refer the reader to a comprehensive analysis of the known higher-mass members by Mentuch et al. (2008) and da Silva et al. (2009).”
BackgroundZuckerman, B., & Webb, R. A. (2000) · The Astrophysical Journal · doi:10.1086/308897 · Cited by 163 · cited 2× · see citing works
“100 Myr) have been identified among the nearby field population (Kastner et al. 1997; Webb et al. 1999; Mamajek et al. 1999; Torres et al. 2000; Zuckerman & Webb 2000; Zuckerman & Song 2004).”
A New Association of Post–T Tauri Stars near the Sun
Torres, C. A. O., da Silva, L., Quast, G. R., Reza, R. D. L., & Jilinski, E. G. (2000) · The Astronomical Journal · doi:10.1086/301539 · Cited by 160 · cited 2× · see citing works
“100 Myr) have been identified among the nearby field population (Kastner et al. 1997; Webb et al. 1999; Mamajek et al. 1999; Torres et al. 2000; Zuckerman & Webb 2000; Zuckerman & Song 2004).”
BackgroundLithium Depletion of Nearby Young Stellar Associations
Cooper, E. M., Brandeker, A., van Kerkwijk, M. H., Jayawardhana, R., & Hauschildt, P. H. (2008) · The Astrophysical Journal · doi:10.1086/592764 · Cited by 157 · cited 4× · see citing works
“Many of the diagnostics of youth have only been firmly calibrated for higher-mass stars (e.g., Mentuch et al. 2008), so our measurements also yield the first robust calibration of isochronal parameter sequences for mid-K to midM dwarfs in Tuc-Hor.”
BackgroundInfluentialStauffer, J. R., Barrado, D., Bouvier, J., Morrison, H. L., Harding, P., Luhman, K. L., Stanke, T., McCaughrean, M., Terndrup, D. M., Allen, L., et al. (1999) · The Astrophysical Journal · doi:10.1086/308069 · Cited by 149 · cited 1× · see citing works
“Barrado y Navascués et al. (2004) reported a boundary at Mbol = 10.24± 0.15 in IC 2391, as well as updating the results of Stauffer et al. (1998, 1999) for α Per (Mbol = 11.31 ± 0.15) and the Pleiades (Mbol = 12.14 ± 0.15).”
ResultInfluentialSEARCHING FOR YOUNG M DWARFS WITHGALEX
Shkolnik, E. L., Liu, M. C., Reid, I. N., Dupuy, T. J., & Weinberger, A. J. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/727/1/6 · Cited by 134 · cited 7× · see citing works
“%) were observed and lie above the FNUV /FJ > 10 −4 threshold used by Shkolnik et al. (2011).”
BackgroundMethodInfluentialSelf-citationExploring Terrestrial Planet Formation in the TW Hydrae Association
Low, F. J., Smith, P. S., Werner, M. W., Chen, C., Krause, V., Jura, M., & Hines, D. C. (2005) · The Astrophysical Journal · doi:10.1086/432640 · Cited by 132 · cited 1× · see citing works
“The low distances also result in additional sensitivity for flux-limited studies of disks (Low et al. 2005; Bouwman et al. 2006; Plavchan et al. 2009) and the (sub)stellar mass function (Gizis 2002; Lyo et al. 2006; Murphy et al. 2010; Shkolnik et al. 2011).”
BackgroundThe lithium depletion boundary in NGC 2547 as a test of pre-main-sequence evolutionary models
Jeffries, R. D., & Oliveira, J. M. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.08820.x · Cited by 125 · see citing works
Randich, S., Pallavicini, R., Meola, G., Stauffer, J. R., & Balachandran, S. C. (2001) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20010339 · Cited by 121 · cited 2× · see citing works
“At an age of τ ∼ 30 Myr, lithium should be completely depleted for stars of SpT K7–M4, but not yet burned for earlier and later types (Randich et al. 2001; Dobbie et al. 2010).”
BackgroundBouwman, J., Lawson, W. A., Dominik, C., Feigelson, E. D., Henning, T. K., Tielens, A. G. G. M., & Waters, L. B. F. M. (2006) · The Astrophysical Journal · doi:10.1086/510365 · Cited by 114 · cited 1× · see citing works
“The low distances also result in additional sensitivity for flux-limited studies of disks (Low et al. 2005; Bouwman et al. 2006; Plavchan et al. 2009) and the (sub)stellar mass function (Gizis 2002; Lyo et al. 2006; Murphy et al. 2010; Shkolnik et al. 2011).”
BackgroundZuckerman, B., Bessell, M. S., Song, I., & Kim, S. (2006) · The Astrophysical Journal · doi:10.1086/508060 · Cited by 114 · cited 1× · see citing works
“50 pc) have subsequently identified several additional populations, including the AB Dor, Carina-Near, HerculesLyra, and Tucana-Horologium associations (Zuckerman & Song 2004; Zuckerman et al. 2006; Torres et al. 2008; Eisenbeiss et al. 2013).”
BackgroundDENIS: A deep near-infrared survey of the southern sky
Epchtein, N., de Batz, B., Copet, E., Fouqué, P., Lacombe, F., Bertre, T. L., Mamon, G. A., Rouan, D., Tiphène, D., Burton, W. B., et al. (1994) · Astrophysics and Space Science · doi:10.1007/bf00990013 · Cited by 113 · cited 1× · see citing works
“DENIS The Deep Near Infrared Survey of the Southern Sky (DENIS; Epchtein et al. 1994) observed ∼84% of the 3 southern sky (with some gaps) in the optical (with a Gunn i filter) and the near-infrared (with J , and Ks filters) during 1995-2001.”
BackgroundClustering of Young Stars in Taurus, Ophiuchus, and the Orion Trapezium
Simon, M. (1997) · The Astrophysical Journal · doi:10.1086/310678 · Cited by 106 · cited 2× · see citing works
“If the former effect dominates, then it would indicate that geometric analyses are of limited use for determining trace-back ages, and more generally that these moving groups formed in a distributed manner (similar to Taurus-Auriga; Simon 1997; Kraus & Hillenbrand 2008) rather than as compact clusters that have since…”
BackgroundTHE GALEX NEARBY YOUNG-STAR SURVEY
Rodriguez, D. R., Zuckerman, B., Kastner, J. H., Bessell, M. S., Faherty, J. K., & Murphy, S. J. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/774/2/101 · Cited by 104 · cited 8× · see citing works
“A similar spatial distribution can be seen in the activityselected candidates reported by Rodriguez et al. (2013).”
BackgroundMethodInfluentialSpatial Distributions of Young Stars
Kraus, A. L., & Hillenbrand, L. A. (2008) · The Astrophysical Journal · doi:10.1086/593012 · Cited by 97 · cited 4× · see citing works
“This trend is consistent with the results of Pecaut et al. (2012), who use several other age diagnostics to determine that the Upper Scorpius subgroup of the Sco-Cen OB association might be a factor of ∼2 older (τ ∼ 11 Myr) than its traditionally accepted isochronal age for low-mass members (τ ∼ 5 Myr; Preibisch et al…”
BackgroundResultInfluentialSelf-citationMeeting the Cool Neighbors. XI. Beyond the NLTT Catalog
Reid, I. N., Cruz, K. L., & Allen, P. (2007) · The Astronomical Journal · doi:10.1086/517914 · Cited by 96 · cited 1× · see citing works
“In Shkolnik et al. (2011) we used the NStars 25-pc census (≈1500 M dwarfs; Reid et al. 2007) to calibrate our GALEX selection criteria.”
MethodDISTANCE AND KINEMATICS OF THE TW HYDRAE ASSOCIATION FROM PARALLAXES
Weinberger, A. J., Anglada-Escudé, G., & Boss, A. P. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/762/2/118 · Cited by 93 · see citing works
A NEW METHOD TO IDENTIFY NEARBY, YOUNG, LOW-MASS STARS
Rodriguez, D. R., Bessell, M. S., Zuckerman, B., & Kastner, J. H. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/727/2/62 · Cited by 90 · cited 3× · see citing works
“…use Previous searches for low-mass YMG members using GALEX used color and proper motion cuts coupled with NUV and/or FUV selection criteria (Shkolnik et al. 2011 and Rodriguez et al. 2011 for TWA and Rodriguez et al. 2013 for Tuc-Hor) before acquiring optical spectra for candidate confirmation.”
BackgroundMethodMAPPING THE SHORES OF THE BROWN DWARF DESERT. III. YOUNG MOVING GROUPS
Evans, T. M., Ireland, M., Kraus, A. L., Martinache, F., Stewart, P. N., Tuthill, P., Lacour, S., Carpenter, J. M., & Hillenbrand, L. A. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/744/2/120 · Cited by 86 · cited 1× · see citing works
“…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).”
BackgroundSelf-citationβ PICTORIS AND AB DORADUS MOVING GROUPS: LIKELY NEW LOW-MASS MEMBERS
Schlieder, J. E., Lépine, S., & Simon, M. (2010) · The Astronomical Journal · doi:10.1088/0004-6256/140/1/119 · Cited by 85 · cited 1× · see citing works
“This method is similar to that used by Lépine & Simon (2009) and Schlieder et al. (2010).”
MethodDeficit of Wide Binaries in the η Chamaeleontis Young Cluster
Brandeker, A., Jayawardhana, R., Khavari, P., Haisch, K. E., & Mardones, D. (2006) · The Astrophysical Journal · doi:10.1086/508483 · Cited by 78 · cited 1× · see citing works
“…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).”
BackgroundKeck Adaptive Optics Imaging of Nearby Young Stars: Detection of Close Multiple Systems
Brandeker, A., Jayawardhana, R., & Najita, J. (2003) · The Astronomical Journal · doi:10.1086/378057 · Cited by 75 · cited 1× · see citing works
“…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).”
BackgroundLIKELY MEMBERS OF THE β PICTORIS AND AB DORADUS MOVING GROUPS IN THE NORTH
Schlieder, J. E., Lépine, S., & Simon, M. (2012) · The Astronomical Journal · doi:10.1088/0004-6256/144/4/109 · Cited by 73 · cited 1× · see citing works
“Schlieder et al. (2012) have already shown that two of these stars are field interlopers, indicating that our more precise proper motions might be better at rejecting field stars that are only moderately discrepant from the proper motion of Tuc-Hor.9 Of the 58 late-type stars identified as…”
BackgroundIC 2602: a lithium depletion boundary age and new candidate low-mass stellar members★
Dobbie, P. D., Lodieu, N., & Sharp, R. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.17355.x · Cited by 71 · cited 2× · see citing works
“At an age of τ ∼ 30 Myr, lithium should be completely depleted for stars of SpT K7–M4, but not yet burned for earlier and later types (Randich et al. 2001; Dobbie et al. 2010).”
BackgroundMethodInfluentialLépine, S., & Simon, M. (2009) · The Astronomical Journal · doi:10.1088/0004-6256/137/3/3632 · Cited by 70 · see citing works
Spectroscopic Abundances in Cool Pleiades Dwarfs and NGC 2264 Stars
King, J. R., Soderblom, D. R., Fischer, D. A., & Jones, B. F. (2000) · The Astrophysical Journal · doi:10.1086/308695 · Cited by 68 · cited 2× · see citing works
“In the canonically ∼125 Myr Pleiades cluster, King et al. (2000) found the boundary to lie at Teff = 4420 K (SpT = K4.”
BackgroundULTRAVIOLET-SELECTED FIELD AND PRE-MAIN-SEQUENCE STARS TOWARD TAURUS AND UPPER SCORPIUS
Findeisen, K. P., & Hillenbrand, L. (2010) · The Astronomical Journal · doi:10.1088/0004-6256/139/4/1338 · Cited by 66 · cited 25× · see citing works
“The GALEX satellite has imaged most of the sky simultaneously in two bands: near-UV (NUV; 1750– 2750 Å) and far-UV (FUV; 1350–1750 Å), with angular resolutions of 5′′ and 6.5′′.”
BackgroundInfluentialKiss, L. L., Moór, A., Szalai, T., Kovács, J., Bayliss, D., Gilmore, G. F., Bienaymé, O., Binney, J., Bland-Hawthorn, J., Campbell, R., et al. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.17660.x · Cited by 62 · see citing works
Law, N. M., Kraus, A. L., Street, R. A., Fulton, B. J., Hillenbrand, L. A., Shporer, A., Lister, T. A., Baranec, C. J., Bloom, J. S., Bui, K., et al. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/757/2/133 · Cited by 54 · see citing works
Self-citationThe Hercules-Lyra association revisited
Eisenbeiß, T., Eiff, M. A., Roell, T., Mugrauer, M., Adam, C., Neuhäuser, R., Schmidt, T. O. B., & Bedalov, A. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201118362 · Cited by 45 · cited 1× · see citing works
“50 pc) have subsequently identified several additional populations, including the AB Dor, Carina-Near, HerculesLyra, and Tucana-Horologium associations (Zuckerman & Song 2004; Zuckerman et al. 2006; Torres et al. 2008; Eisenbeiss et al. 2013).”
BackgroundA deep photometric survey of the η Chamaeleontis cluster down to the brown dwarf – planet boundary
Lyo, A.-R., Song, I., Lawson, W. A., Bessell, M. S., & Zuckerman, B. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.10232.x · Cited by 43 · cited 1× · see citing works
“The low distances also result in additional sensitivity for flux-limited studies of disks (Low et al. 2005; Bouwman et al. 2006; Plavchan et al. 2009) and the (sub)stellar mass function (Gizis 2002; Lyo et al. 2006; Murphy et al. 2010; Shkolnik et al. 2011).”
BackgroundIDENTIFICATION OF THE LITHIUM DEPLETION BOUNDARY AND AGE OF THE SOUTHERN OPEN CLUSTER BLANCO 1
Cargile, P. A., James, D. J., & Jeffries, R. D. (2010) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/725/2/l111 · Cited by 43 · cited 1× · see citing works
“Cargile et al. (2010) reported a boundary for Blanco 1 at Mbol = 11.99± 0.30.”
BackgroundInfluentialProper‐Motion Catalog from SDSS ∩ USNO‐B
Gould, A. P., & Kollmeier, J. A. (2004) · The Astrophysical Journal Supplement Series · doi:10.1086/382529 · Cited by 40 · cited 1× · see citing works
“…have employed various combinations of all-sky surveys in order to systematically measure proper motions of both clusters and field stars; USNOB is itself a product of such analysis, Gould & Kollmeier (2004) combined SDSS and USNOB, and the PPMXL survey (Roeser et al. 2010) combined 2MASS and USNOB.”
MethodX-ray view of IC 348 in the light of an updated cluster census
Stelzer, B., Preibisch, T., Alexander, F., Mucciarelli, P., Flaccomio, E., Micela, G., & Sciortino, S. (2011) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201118118 · Cited by 38 · cited 1× · see citing works
“Also, activity signatures show wide variations in any single-aged population (Stelzer et al. 2012, Shkolnik & Barman, in preparation), though some show a lower bound that allows for dispositive rejection of nonmembers.”
BackgroundLithium abundances in the α Per cluster
Balachandran, S. C., Mallik, S. V., & Lambert, D. L. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.17630.x · Cited by 32 · see citing works
First detection of a low-mass stellar halo around the young open cluster η Chamaeleontis
Murphy, S. J., Lawson, W. A., & Bessell, M. S. (2010) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1111/j.1745-3933.2010.00879.x · Cited by 27 · see citing works
Spectroscopy of Active and Inactive M Dwarfs in Praesepe
Kafka, S., & Honeycutt, R. K. (2006) · The Astronomical Journal · doi:10.1086/506561 · Cited by 27 · cited 1× · see citing works
“• Hα emission: Old main sequence stars exhibit a wide range of activity levels (e.g., Kafka & Honeycutt 2006; West et al. 2011), and hence the presence of strong Hα emission can not be used as a positive criterion for determining membership.”
BackgroundZacharias, N. (2010) · The Astronomical Journal · doi:10.1088/0004-6256/139/6/2208 · Cited by 14 · cited 1× · see citing works
“We have addressed this problem by adopting proper motions for bright stars as measured by the Third USNO CCD Astrograph Catalog (UCAC3; Zacharias 2010).”
Method
Flagged first, then by citations
Research works printed but not linked: 2
- Rucinski, S. 1999, in ASP Conf. Ser. 185, IAU Colloq. 170: Precise Stellar Radial Velocities, ed. J. B. Hearnshaw & C. D. Scarfe (San Francisco, CA: ASP), 82
- Schmidt-Kaler, T. 1982, Landolt-Bornstein Numerical Data and Functional Relationships in Science and Technology, New Series, Group VI, Vol. 2b (Berlin: Springer)
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 · see citing works
“…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 · see citing works
“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. (2016) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/128/968/102001 · Cited by 365 · see citing works
“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 · see citing works
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 · see citing works
“0 (Monet et al. 2003), as described in Kraus & Hillenbrand (2007) and Kraus et al. (2014), to estimate both parameters.”
BackgroundSelf-citationTHE HAWAII INFRARED PARALLAX PROGRAM. II. YOUNG ULTRACOOL FIELD DWARFS
Liu, M. C., Dupuy, T., & Allers, K. (2016) · The Astrophysical Journal · doi:10.3847/1538-4357/833/1/96 · Cited by 207 · see citing works
“…to find young ultracool dwarfs in the nearest young moving groups through kinematic and stellar-activity criteria (e.g., Shkolnik et al. 2009, 2011, 2012; Rodriguez et al. 2011; Schlieder et al. 2012; Malo et al. 2013; Gagné et al. 2014b; Kraus et al. 2014; Gagné et al. 2015b; Aller et al. 2016).”
BackgroundSelf-citationGagné, J., Faherty, J. K., Cruz, K. L., Lafreniére, D., Doyon, R., Malo, L., Burgasser, A. J., Naud, M.-È., Artigau, É., Bouchard, S., et al. (2015) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/219/2/33 · Cited by 223 · see citing works
“…2001a; Malo et al. 2014b; Binks & Jeffries 2014), Tucana-Horologium (THA; 20–40 Myr; Torres et al. 2000; Zuckerman & Webb 2000; Zuckerman et al. 2001b; Kraus et al. 2014b), Carina (CAR; 20–40 Myr; Torres et al. 2008), Columba (COL; 20–40 Myr; Torres et al. 2008), Argus (ARG; 30–50 Myr; Makarov…”
BackgroundMethodResultInfluentialPLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS
Bowler, B., Liu, M. C., Shkolnik, E., & Tamura, M. (2014) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/216/1/7 · Cited by 158 · see citing works
“Similarly, Kraus et al. (2014) infer a Li-depletion age of ≈40 Myr for the Tuc-Hor moving group, which is roughly 10 Myr older than its age from isochrone fitting.”
BackgroundSelf-citationIndividual Dynamical Masses of Ultracool Dwarfs* † ‡
Dupuy, T. J., & Liu, M. C. (2017) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/aa5e4c · Cited by 200 · see citing works
“Lithium Fusion Mass Limit Theoretical predictions of lithium depletion in ultracool dwarfs as a function of mass and age are thought to be one of the most reliable methods for age-dating young clusters (e.g., Chabrier et al. 1996; Bildsten et al. 1997; Binks & Jeffries 2014; Kraus et al. 2014).”
MethodSelf-citationMann, A. W., Gaidos, E. J., Mace, G. N., Johnson, M. C., Bowler, B. P., LaCourse, D. M., Jacobs, T. L., Vanderburg, A. M., Kraus, A. L., Kaplan, K., et al. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/818/1/46 · Cited by 182 · see citing works
“Distance: Because K2-25 is a member of the Hyades, we can derive a kinematic distance more precise than the photometric distance we used in Section 3 (e.g., Kraus et al. 2014).”
MethodSelf-citationHAZMAT. I. THE EVOLUTION OF FAR-UV AND NEAR-UV EMISSION FROM EARLY M STARS
Shkolnik, E. L., & Barman, T. S. (2014) · The Astronomical Journal · doi:10.1088/0004-6256/148/4/64 · Cited by 169 · see citing works
“…al. (2003), 10: Reid (2003), 11: Jayawardhana et al. (2006), 12: Zuckerman et al. (2001), 13: Looper et al. (2010), 14: Shkolnik et al. (2012), 15: Kraus et al. (2014), 16: Montes et al. (2001), 17: Zuckerman et al. (2004), 18: Malo et al. (2013), 19: López-Santiago et al. (2006), 20: Bowler et…”
BackgroundSelf-citationNewton, E. R., Mann, A. W., Tofflemire, B. M., Pearce, L., Rizzuto, A. C., Vanderburg, A. M., Martinez, R. A., Wang, J. J., Ruffio, J.-B., Kraus, A. L., et al. (2019) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ab2988 · Cited by 164 · see citing works
Self-citationCORRECTING FOR TELLURIC ABSORPTION: METHODS, CASE STUDIES, AND RELEASE OF THE TelFit CODE
Gullikson, K., Dodson-Robinson, S., & Kraus, A. (2014) · The Astronomical Journal · doi:10.1088/0004-6256/148/3/53 · Cited by 146 · see citing works
“The reduced spectra were wavelength calibrated using a combination of a ThAr lamp exposure and the 760 nm telluric A band (see Kraus et al. 2014, for details).”
MethodSelf-citationMalo, L., Doyon, R., Feiden, G. A., Albert, L., Lafreniére, D., Artigau, É., Gagné, J., & Riedel, A. R. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/792/1/37 · Cited by 142 · see citing works
“…young low-mass stars that have been unambiguously identified in the solar neighborhood, though the number of candidates is rapidly increasing (e.g., Kraus et al. 2014; Riedel et al. 2014; Malo et al. 2013; Rodriguez et al. 2013; Shkolnik et al. 2012; Rodriguez et al. 2011; Torres et al. 2008;…”
BackgroundEMPIRICAL ISOCHRONES FOR LOW MASS STARS IN NEARBY YOUNG ASSOCIATIONS
(沈雷歌), G. J. H., & Hillenbrand, L. A. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/808/1/23 · Cited by 136 · see citing works
“In recent years, the growing number of proper motions and parallax distances have led to a substantial improvement in the accounting of membership within young associations (e.g. Malo et al. 2013; Kraus et al. 2014).”
BackgroundMethodInfluentialBANYAN. XIII. A First Look at Nearby Young Associations with Gaia Data Release 2
Gagn'e, J., & Faherty, J. (2018) · Astrophysical Journal · doi:10.3847/1538-4357/aaca2e · Cited by 87 · see citing works
“Previous searches for new low-mass members in these young associations (e.g., Rodriguez et al. 2011; Shkolnik et al. 2012, 2017; Malo et al. 2013; Kraus et al. 2014) identified only a fraction of the mid-to-late-M dwarfs because of their faintness and the need to obtain follow-up trigonometric…”
BackgroundResultGagné, J., Lafreniére, D., Doyon, R., Malo, L., & Artigau, É. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/798/2/73 · Cited by 131 · see citing works
“Subsequently, Kraus et al. (2014) and Malo et al. (2014a) independently measured RVs of 4.0 ± 2.0 km s−1 and 7.3 ± 2.6 km s−1 respectively, whereas the latter independently identifies it as a candidate member of THA.”
BackgroundMethodInfluentialThe International Deep Planet Survey
Galicher, R., Marois, C., Macintosh, B., Zuckerman, B., Barman, T., Konopacky, Q., Song, I., Patience, J., Lafreniére, D., Doyon, R., et al. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201527828 · Cited by 130 · see citing works
All-sky Co-moving Recovery Of Nearby Young Members (ACRONYM). II. The β Pictoris Moving Group∗
Shkolnik, E. L., Allers, K., Kraus, A. L., Liu, M. C., & Flagg, L. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa77fa · Cited by 118 · see citing works
“A test of this selection process in our Tuc-Hor search (Kraus et al. 2014) showed that applying a GALEX selection criterion to candidates is indeed more efficient, leading to a higher confirmation rate for spectroscopic follow-up.”
BackgroundMethodResultInfluentialSelf-citationKerr, R. M. P., Rizzuto, A. C., Kraus, A. L., & Offner, S. S. R. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac0251 · Cited by 112 · see citing works
Self-citationTESS Reveals that the Nearby Pisces–Eridanus Stellar Stream is only 120 Myr Old
Curtis, J. L., Agüeros, M. A., Mamajek, E. E., Wright, J. T., & Cummings, J. D. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab2899 · Cited by 104 · see citing works
Frasca, A., Biazzo, K., Lanzafame, A. C., Alcalá, J. M., Brugaletta, E., Klutsch, A., Stelzer, B., Sacco, G. G., Spina, L., Jeffries, R. D., et al. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201424409 · Cited by 101 · see citing works
“This behavior is commonly observed in young clusters and associations (see, e.g. Stauffer et al. 1997; Kraus et al. 2014).”
BackgroundDesidera, S., Covino, E., Messina, S., Carson, J., Hagelberg, J., Schlieder, J., Biazzo, K., Alcalá, J., Chauvin, G., Vigan, A., et al. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201323168 · Cited by 70 · see citing works
Krolikowski, D. M., Kraus, A. L., & Rizzuto, A. C. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/ac0632 · Cited by 98 · see citing works
Self-citationThe Greater Taurus–Auriga Ecosystem. I. There is a Distributed Older Population
Kraus, A. L., Herczeg, G. J., Rizzuto, A. C., Mann, A. W., Slesnick, C. L., Carpenter, J. M., Hillenbrand, L. A., & Mamajek, E. E. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa62a0 · Cited by 96 · see citing works
“We therefore have iden- tified an upper envelope for lithium equivalent widths, calibrated with the Tuc-Hor sequence, that identifies objects with SpT = K3–M4 as being notably young (τ .”
BackgroundMethodResultInfluentialSelf-citationKraus, A. L., Cody, A. M., Covey, K. R., Rizzuto, A. C., Mann, A. W., & Ireland, M. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/807/1/3 · Cited by 95 · see citing works
“Our analysis of the HIRES data is very similar to the methods described in Kraus et al. (2011b) and Kraus et al. (2014).”
BackgroundMethodSelf-citationLACEwING: A New Moving Group Analysis Code
Riedel, A. R., Blunt, S. C., Lambrides, E., Rice, E. L., Cruz, K. L., & Faherty, J. K. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/153/3/95 · Cited by 91 · see citing works
“These kinematic distances are compared to spectroscopic, photometric or trigonometric distances (Lépine & Simon 2009) or with spectrophotometric distances and a distance modulus cutoff to enforce the stars falling on the approximately correct isochrone (Kraus et al. 2014a).”
BackgroundMethodResultInfluentialHAZMAT. IV. Flares and Superflares on Young M Stars in the Far Ultraviolet*
Loyd, R. O. P., Shkolnik, E. L., Schneider, A. C., Barman, T., Meadows, V., Pagano, I., & Peacock, S. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aae2ae · Cited by 87 · see citing works
“The stars in the sample were identified as members of the Tuc-Hor association using 3D space velocities and youth indicators by Shkolnik et al. (2011, 2012) and Kraus et al. (2014).”
BackgroundMethodSelf-citationA Warm Jupiter-sized Planet Transiting the Pre-main-sequence Star V1298 Tau
David, T. J., Cody, A. M., Hedges, C., Mamajek, E. E., Hillenbrand, L. A., Ciardi, D. R., Beichman, C. A., Petigura, E. A., Fulton, B. J., Isaacson, H. T., et al. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab290f · Cited by 86 · see citing works
THE BROWN DWARF KINEMATICS PROJECT (BDKP). IV. RADIAL VELOCITIES OF 85 LATE-M AND L DWARFS WITH MagE
Burgasser, A. J., Logsdon, S. E., Gagné, J., Bochanski, J. J., Faherty, J. K., West, A. A., Mamajek, E. E., Schmidt, S. J., & Cruz, K. L. (2015) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/220/1/18 · Cited by 82 · see citing works
“…Mamajek & Bell 2014, Malo et al. 2014, Binks & Jeffries 2014), the Tucana-Horologium Association (THA; Torres et al. 2000, Zuckerman & Webb 2000; 40 Myr; Kraus et al. 2014), the Carina association (CAR; 20 – 40 Myr; Torres et al. 2008), the Columba association (COL; 20 – 40 Myr; Torres et al.…”
BackgroundHoward, W. S., & MacGregor, M. A. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac426e · Cited by 82 · see citing works
Howard, W. S., Corbett, H., Law, N. M., Ratzloff, J. K., Galliher, N., Glazier, A., Gonzalez, R., Soto, A. V., Fors, O., del Ser, D., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abb5b4 · Cited by 81 · see citing works
“Most of the SIMBAD types were identified by several spectroscopic surveys (e.g. Henry et al. 2002, 2006; Riaz et al. 2006; Torres et al. 2006; Kraus et al. 2014; Gaidos et al. 2014; Riedel et al. 2017).”
BackgroundHoward, W. S., Corbett, H., Law, N. M., Ratzloff, J. K., Glazier, A., Fors, O., del Ser, D., & Haislip, J. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab2767 · Cited by 80 · see citing works
The Gaia-ESO Survey: empirical estimates of stellar ages from lithium equivalent widths ( eagles )
Jeffries, R. D., Jackson, R. J., Wright, N. J., Weaver, G., Gilmore, G. F., Randich, S., Bragaglia, A., Korn, A. J., Smiljanić, R., Biazzo, K., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1293 · Cited by 80 · see citing works
Bouma, L. G., Hartman, J. D., Bhatti, W. A., Winn, J. N., & Bakos, G. Á. (2019) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ab4a7e · Cited by 76 · see citing works
“The Kraus et al. (2014), Röser et al. (2011), and Bell et al. (2017) studies reported members in Tucana-Horologium, the Hyades, and 32Ori respectively.”
BackgroundResultBANYAN. XII. New Members of Nearby Young Associations from GAIA–Tycho Data
Gagné, J., Roy-Loubier, O., Faherty, J. K., Doyon, R., & Malo, L. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aac2b8 · Cited by 71 · see citing works
“…well as radial velocities and parallaxes when available (e.g., see Mamajek 2005; Rodriguez et al. 2011; Malo et al. 2013, 2014; Gagné et al. 2014; Kraus et al. 2014; Gagné et al. 2015b; Murphy & Lawson 2015; Riedel et al. 2017; Shkolnik et al. 2017), and have started to uncover and confirm the…”
BackgroundCurrie, T., Brandt, T. D., Uyama, T., Nielsen, E. L., Blunt, S. C., Guyon, O., Tamura, M., Marois, C., Mede, K., Kuzuhara, M., et al. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aae9ea · Cited by 65 · see citing works
The SPHERE infrared survey for exoplanets (SHINE)
Desidera, S., Chauvin, G., Bonavita, M., Messina, S., Coroller, H. L., Schmidt, T. O. B., Gratton, R., Lazzoni, C., Meyer, M., Schlieder, J., et al. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038806 · Cited by 67 · see citing works
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) · The Astronomical Journal · doi:10.3847/1538-3881/abdf53 · Cited by 65 · see citing works
“If the siblings of HD 110082 remain sufficiently concentrated, their presence should be apparent as a recognizable spatial over-density on the sky, as can be seen for the kinematic candidate members of nearby young moving groups like Tucana-Horologium (Kraus et al. 2014).”
BackgroundMethodInfluentialSelf-citationBowler, B. P., Tran, Q. H., Zhang, Z., Morgan, M., Ashok, K. B., Blunt, S. C., Bryan, M. L., Evans, A. E., Franson, K., Huber, D., et al. (2023) · The Astronomical Journal · doi:10.3847/1538-3881/acbd34 · Cited by 65 · see citing works
“A faint companion was found with HST imaging by White & Ghez (2001) and confirmed to be comoving by Kraus et al. (2014a); however, follow-up studies suggest FW Tau C may be a brown dwarf or a low-mass star with an edge-on disk (Bowler et al. 2014; Caceres et al. 2015; Kraus et al. 2015; Wu &…”
BackgroundInfluentialHoward, W. S., Corbett, H., Law, N. M., Ratzloff, J. K., Galliher, N., Glazier, A., Gonzalez, R., Vasquez Soto, A., Fors Aldrich, O., Ser Badia, D. D., et al. (2020) · Dipòsit Digital de la Universitat de Barcelona (Universitat de Barcelona) · Cited by 63 · see citing works
HAZMAT. III. The UV Evolution of Mid- to Late-M Stars with GALEX
Schneider, A. C., & Shkolnik, E. L. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aaaa24 · Cited by 62 · see citing works
“Distances for the 8 pc sample come from Kirkpatrick et al. (2012), while distances for young moving group members come from Kraus et al. (2014), Bell et al. (2015), Gagné et al. (2017), and Shkolnik et al. (2017).”
BackgroundSelf-citationNew low-mass members of the Octans stellar association and an updated 30–40 Myr lithium age
Murphy, S. J., & Lawson, W. A. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu2450 · Cited by 61 · see citing works
“8), which has recently had a lithium depletion boundary (LDB) age of 40 ± 2 Myr estimated by Kraus et al. (2014).”
BackgroundMethodResultInfluentialA possibly inflated planet around the bright young star DS Tucanae A
Benatti, S., Nardiello, D., Malavolta, L., Desidera, S., Borsato, L., Nascimbeni, V., Damasso, M., D’Orazi, V., Mesa, D., Messina, S., et al. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201935598 · Cited by 61 · see citing works
“The observed RV dispersion of DS Tuc A is within the range of dispersion for stars with similar age and spectral type, derived from HARPS spectra of several objects available in the ESO archive, further supporting the magnetic activity as the dominant source of variability (e.g. Kraus et al. 2014).”
BackgroundMethodInfluentialTwo Young Planetary Systems around Field Stars with Ages between 20 and 320 Myr from TESS
Zhou, G., Quinn, S. N., Irwin, J., Huang, C. X., Collins, K. A., Bouma, L. G., Khan, L., Landrigan, A., Vanderburg, A. M., Rodriguez, J. E., et al. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/abba22 · Cited by 60 · see citing works
HAZMAT VI: The Evolution of Extreme Ultraviolet Radiation Emitted from Early M Stars
Peacock, S., Barman, T., Shkolnik, E. L., Loyd, R. O. P., Schneider, A. C., Pagano, I., & Meadows, V. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab893a · Cited by 58 · see citing works
Self-citationHoward, W. S., Corbett, H., Law, N. M., Ratzloff, J. K., Glazier, A., Fors Aldrich, O., Ser Badia, D. D., & Haislip, J. (2019) · Dipòsit Digital de la Universitat de Barcelona (Universitat de Barcelona) · Cited by 59 · see citing works
Calibration of the Hα Age–Activity Relation for M Dwarfs
Kiman, R., Faherty, J. K., Cruz, K. L., Gagné, J., Angus, R., Schmidt, S. J., Mann, A. W., Gagliuffi, D. C. B., & Rice, E. L. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/abf561 · Cited by 59 · see citing works
Schneider, A. C., Shkolnik, E. L., Allers, K., Kraus, A. L., Liu, M. C., Weinberger, A. J., & Flagg, L. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab1a26 · Cited by 59 · see citing works
Self-citationA Warm Jupiter-sized Planet Transiting the Pre-main-sequence Star V1298 Tau
David, T. J., Cody, A. M., Hedges, C., Mamajek, E. E., Hillenbrand, L. A., Ciardi, D. R., Beichman, C., Petigura, E. A., Fulton, B. J., Isaacson, H. T., et al. (2019) · eScholarship (California Digital Library) · Cited by 59 · see citing works
MASSIVE: A Bayesian analysis of giant planet populations around low-mass stars
Lannier, J., Delorme, P., Lagrange, A. ‐., Borgniet, S., Rameau, J., Schlieder, J. E., Gagné, J., Bonavita, M., Malo, L., Chauvin, G., et al. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201628237 · Cited by 57 · see citing works
“…2014; Malo et al. 2014b; Mamajek & Bell 2014), 8 stars from Tucana-Horologium (20-40 Myr; we use 30 Myr, hereafter THA, Zuckerman & Webb 2000; Kraus et al. 2014b), 3 stars from Columba (20-40 Myr; we use 30 Myr, hereafter COL, Torres et al. 2008), 1 star from Argus (30-50 Myr; we use 40…”
MethodAnalysis of Membership Probability in Nearby Young Moving Groups with Gaia DR2
Ujjwal, K., Kartha, S. S., Mathew, B., Manoj, P., & Narang, M. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/ab76d6 · Cited by 55 · see citing works
Binks, A. S., & Jeffries, R. D. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2431 · Cited by 54 · see citing works
“We find the B14 isochrones best match the BPMG and ABDMG sequence and agree with recent LDB ages for both the BPMG (Binks & Jeffries 2014) and TucanaHorologium (Kraus et al. 2014; Bell, Mamajek & Naylor 2015).”
ResultSearch for associations containing young stars (SACY)
Elliott, P., Bayo, A., Melo, C., Torres, C. A. O., Sterzik, M., Quast, G. R., Montes, D., & Brahm, R. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201628253 · Cited by 54 · see citing works
“…high-probability members from a collection of prominent moving group works to date (Torres et al. 2008; Zuckerman et al. 2011; Malo et al. 2014; Kraus et al. 2014; Elliott et al. 2014; Murphy & Lawson 2015), which cover a wide range of spectral types (B2-M5) and ages (∼5-150 Myr), totalling…”
BackgroundMethodResultInfluentialStrong Hα emission and signs of accretion in a circumbinary planetary mass companion from MUSE
Ringqvist, S. C., Torres, R. A., Janson, M., Aoyama, Y., Marleau, G.-D., Bonnefoy, M., & Petrus, S. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038131 · Cited by 52 · see citing works
“Several works assign Delorme 1 to the THA (e.g. Kraus et al. 2014; Malo et al. 2014; Gagné et al. 2015), while Riedel et al. (2014) noted that the over-luminosity of both Delorme 1 A and B indicates an even younger age.”
BackgroundReaching the boundary between stellar kinematic groups and very wide binaries
Alonso-Floriano, F. J., Caballero, J. A., Cortés‐Contreras, M., Solano, E., & Montes, D. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201526795 · Cited by 50 · see citing works
A Well-aligned Orbit for the 45 Myr-old Transiting Neptune DS Tuc Ab
Zhou, G., Winn, J. N., Newton, E. R., Quinn, S. N., Rodriguez, J. E., Mann, A. W., Rizzuto, A. C., Vanderburg, A. M., Huang, C. X., Latham, D. W., et al. (2020) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ab7d3c · Cited by 49 · see citing works
“The age of the star is constrained by a Gaussian prior of 45±4Myr, based on the age of the TucanaHorologium moving group (Kraus et al. 2014; Bell et al. 2015).”
BackgroundTwo Young Planetary Systems around Field Stars with Ages between 20 and 320 Myr from TESS
Zhou, G., Quinn, S. N., Irwin, J. M., Huang, C. X., Collins, K. A., Bouma, L. G., Khan, L., Landrigan, A., Vanderburg, A. M., Rodriguez, J. E., et al. (2020) · Keele Research Repository (Keele University) · Cited by 48 · see citing works
Search for associations containing young stars (SACY)
Zúñiga-Fernández, S., Bayo, A., Elliott, P., Zamora, C., Corvalán, G., Haubois, X., Corral-Santana, J. M., Olofsson, J., Huélamo, N., Sterzik, M., et al. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202037830 · Cited by 47 · see citing works
Nardiello, D., Malavolta, L., Desidera, S., Baratella, M., D’Orazi, V., Messina, S., Biazzo, K., Benatti, S., Damasso, M., Rajpaul, V., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243743 · Cited by 46 · see citing works
Gaidos, E. J., Mann, A. W., Rizzuto, A. C., Nofi, L., Mace, G. N., Vanderburg, A. M., Feiden, G. A., Narita, N., Takeda, Y., Esposito, T. M., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2345 · Cited by 46 · see citing works
Self-citationWISE J080822.18−644357.3 – a 45 Myr-old accreting M dwarf hosting a primordial disc
Murphy, S. J., Mamajek, E. E., & Bell, C. P. M. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty471 · Cited by 47 · see citing works
“Unlike Carina, which is a particularly sparse association of a few dozen highprobability members (see Section 3.1), Tuc-Hor contains hundreds of stars (Kraus et al. 2014).”
BackgroundInfluentialDupuy, T. J., Forbrich, J., Rizzuto, A. C., Mann, A. W., Aller, K., Liu, M. C., Kraus, A. L., & Berger, E. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/827/1/23 · Cited by 44 · see citing works
“…empirical boundary that can be used as a relative age scale between different clusters, and evolutionary models can be used to infer absolute ages of individual clusters based on the location of this lithium depletion boundary (e.g., Bildsten et al. 1997; Binks & Jeffries 2014; Kraus et al. 2014).”
BackgroundSelf-citationBowler, B. P., Hinkley, S., Ziegler, C., Baranec, C., Gizis, J. E., Law, N. M., Liu, M. C., Shah, V. S., Shkolnik, E. L., Riaz, B., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab1018 · Cited by 44 · see citing works
Self-citationUsing rotation, magnetic activity and lithium to estimate the ages of low mass stars
Jeffries, R. D. (2014) · EAS Publications Series · doi:10.1051/eas/1465008 · Cited by 43 · see citing works
“…to groups of stars in clusters (see Table 1 in Soderblom et al. 2013), but has also been applied to spatially dispersed members of young kinematic groups (the Beta Pic group with an LDB age of 21 ± 4Myr, Binks & Jeffries 2014; the Tuc-Hor group with an LDB age of 41±2Myr, Kraus et al. 2014).”
Artigau, É., Gagn'e, J., Faherty, J., Malo, L., Naud, M., Doyon, R., Lafrèniere, D., & Beletsky, Y. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/806/2/254 · Cited by 23 · see citing works
“First, it is part of the 129 new late-type (K3 and later) THA members identified by Kraus et al. 2014; their membership being established by Li and RV measurements, but lack parallaxes and is based on spectroscopic distances.”
BackgroundMethodInfluentialMessina, S., Millward, M., Buccino, A. P., Zhang, L., Medhi, B. J., Jofré, E., Petrucci, R., Pi, Q., Hambsch, F.-J., Kehusmaa, P., et al. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201629152 · Cited by 42 · see citing works
“Malo et al. (2014a) measured a projected rotational velocity v sin i = 11.5±1.4 km s−1, whereas Kraus et al. (2014) measured v sin i = 6.8±0.6 km s−1.”
BackgroundInfluentialDupuy, T., Liu, M. C., Allers, K., Biller, B., Kratter, K., Mann, A., Shkolnik, E., Kraus, A., & Best, W. (2018) · Astronomical Journal · doi:10.3847/1538-3881/aacbc2 · Cited by 36 · see citing works
Self-citationDeacon, N. R., Kraus, A. L., Mann, A. W., Magnier, E. A., Chambers, K. C., Wainscoat, R. J., Tonry, J. L., Kaiser, N., Waters, C. Z., Flewelling, H., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2132 · Cited by 41 · see citing works
“Rotations periods from McQuillan et al. (2014) Key: a proper motion from Zacharias et al. (2013), bSED fit calculated using the methods of Kraus et al. (2014a),c proper motion/SED fit from this work, d proper motion from Roeser et al. (2010) .”
BackgroundMethodInfluentialSelf-citationKraus, A. L., Douglas, S. T., Mann, A. W., Agüeros, M. A., Law, N. M., Covey, K. R., Feiden, G. A., Rizzuto, A. C., Howard, A. W., Isaacson, H., et al. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa7e75 · Cited by 40 · see citing works
“Our analysis of the HIRES data to measure RVs is identical to the methods described in Kraus et al. (2011, 2014, 2015).”
MethodSelf-citationA Well-aligned Orbit for the 45 Myr-old Transiting Neptune DS Tuc Ab
Zhou, G., Winn, J. N., Newton, E. R., Quinn, S. N., Rodriguez, J. E., Mann, A. W., Rizzuto, A. C., Vanderburg, A. M., Huang, C. X., Latham, D. W., et al. (2020) · Cited by 40 · see citing works
Lithium depletion boundary, stellar associations, andGaia
Galindo-Guil, F. J., Barrado, D., Bouy, H., Olivares, J., Bayo, A., Morales‐Calderón, M., Huélamo, N., Sarro, L. M., Riviére-Marichalar, P., Stoev, H., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202141114 · Cited by 40 · see citing works
Houdebine, E. R., Mullan, D. J., Doyle, J. G., de la Vieuville, G., Butler, C. J., & Paletou, F. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab23fe · Cited by 39 · see citing works
The μ Tau Association: A 60 Myr Old Coeval Group at 150 pc from the Sun
Gagné, J., David, T. J., Mamajek, E. E., Mann, A. W., Faherty, J. K., & Bédard, A. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abb77e · Cited by 39 · see citing works
“The lithium depletion boundary has therefore become a popular diagnostic tool to determine precise ages for stellar populations with known M-type stars (e.g., Kraus et al. 2014; Malo et al. 2014b; Shkolnik et al. 2017).”
BackgroundMethodInfluentialGiant white-light flares on fully convective stars occur at high latitudes
Ilin, E., Poppenhaeger, K., Schmidt, S. J., Järvinen, S. P., Newton, E. R., Alvarado‐Gómez, J. D., Pineda, J. S., Davenport, J. R. A., Oshagh, M., & Ilyin, I. V. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2159 · Cited by 39 · see citing works
BANYAN. VIII. NEW LOW-MASS STARS AND BROWN DWARFS WITH CANDIDATE CIRCUMSTELLAR DISKS
Boucher, A., Lafreniére, D., Gagné, J., Malo, L., Faherty, J. K., Doyon, R., & Chen, C. H. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/832/1/50 · Cited by 38 · see citing works
“…Malo et al. 2014b; Binks & Jeffries 2014), Tucana-Horologium (THA; 41− 49Myr; American & Society 2000; Zuckerman & Webb 2000; Zuckerman et al. 2001b; Kraus et al. 2014), Carina (CAR; 38− 56Myr; Torres et al. 2008), Columba (COL; 38− 48Myr; Torres et al. 2008), Argus (ARG; 61− 88Myr; Makarov &…”
BackgroundInfluentialDirect imaging of molten protoplanets in nearby young stellar associations
Bonati, I., Lichtenberg, T., Bower, D. J., Timpe, M., & Quanz, S. P. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833158 · Cited by 36 · see citing works
“A-, G-, and M-star members: (1) Mamajek & Bell (2014), (2) Torres et al. (2008), (3) Zuckerman et al. (2011), (4) Wenger et al. (2000), (5) Kraus et al. (2014), (6) Gagné et al. (2017), (7) Bell et al. (2017), (8) Shvonski et al. (2016), (9) Mamajek (2016).”
Discovery of a Transiting Adolescent Sub-Neptune Exoplanet with K2
David, T. J., Mamajek, E. E., Vanderburg, A. M., Schlieder, J. E., Bristow, M., Petigura, E. A., Ciardi, D. R., Crossfield, I. J. M., Isaacson, H. T., Cody, A. M., et al. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aaeed7 · Cited by 37 · see citing works
“Young, low-mass stars have been shown to exhibit significant emission above photospheric levels in the near-UV (NUV, 1750–2750Å) and far-UV (FUV, 1350–1750Å) GALEX passbands (Findeisen & Hillenbrand 2010; Rodriguez et al. 2011, 2013; Shkolnik et al. 2011; Kraus et al. 2014).”
BackgroundMethodInfluentialHAZMAT. V. The Ultraviolet and X-Ray Evolution of K Stars
Richey-Yowell, T., Shkolnik, E. L., Schneider, A. C., Osby, E., Barman, T., & Meadows, V. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aafa74 · Cited by 37 · see citing works
Self-citationWood, M., Mann, A., Barber, M. G., Bush, J. L., Kraus, A., Tofflemire, B., Vanderburg, A., Newton, E., Feiden, G., Zhou, G., et al. (2022) · Astronomical Journal · doi:10.3847/1538-3881/aca8fc · Cited by 29 · see citing works
Self-citationMass and period limits on the ringed companion transiting the young star J1407
Kenworthy, M. A., Lacour, S., Kraus, A., Triaud, A. H. M. J., Mamajek, E. E., Scott, E. L., Ségransan, D., Ireland, M., Hambsch, F.-J., Reichart, D. E., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu2067 · Cited by 36 · see citing works
“Finally, we used the procedures described in Kraus et al. (2014) to estimate the spectral type and measure vrad, v sin(i?)”
BackgroundMethodSelf-citationDurkan, S., Janson, M., & Carson, J. C. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/824/1/58 · Cited by 33 · see citing works
“…proves difficult to explain, their existence has been confirmed with the detection of several planetary mass companions e.g. 1RXS J16092105 b; 330 AU (Lafrenière et al. 2010), FW Tau b; 330 AU (Kraus et al. 2014a), HD106906 b; 650 AU (Bailey et al. 2014), GU Psc b; 2000 AU (Naud et al. 2014).”
BackgroundBinaries among low-mass stars in nearby young moving groups
Janson, M., Durkan, S., Hippler, S., Dai, X., Brandner, W., Schlieder, J., Bonnefoy, M., & Henning, T. K. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201629945 · Cited by 35 · see citing works
“Here, we present the results of a high-resolution imaging survey of low-mass stars that have been identified as probable members of nearby YMGs (Malo et al., 2013, 2014; Kraus et al., 2014), primarily motivated by the reasoning above.”
BackgroundMethodInfluentialA stellar census of the nearby, young 32 Orionis group
Bell, C. P. M., Murphy, S. J., & Mamajek, E. E. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx535 · Cited by 35 · see citing works
“We therefore adopt the observational criteria described in Luhman & Mamajek (2012) which has been used in several recent studies of nearby young moving groups and associations (see e.g. Kraus et al. 2014; Pecaut & Mamajek 2016).”
BackgroundMethodInfluentialK2 Ultracool Dwarfs Survey – V. High superflare rates on rapidly rotating late-M dwarfs
Paudel, R. R., Gizis, J. E., Mullan, D. J., Schmidt, S. J., Burgasser, A. J., Williams, P. K. G., Youngblood, A. A., & Stassun, K. G. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz886 · Cited by 34 · see citing works
“The latter star (hereafter GSC) differs from our target star 2M0837+2050 in that it is warmer (sp. type = M2, Teff ∼ 3440 K; Pecaut & Mamajek 2013) and younger (∼40 Myr; Kraus et al. 2014).”
BackgroundNew Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Moranta, L., Gagné, J., Couture, D., & Faherty, J. K. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac8c25 · Cited by 34 · see citing works
Addressing Systematics in the Traceback Age of the β Pictoris Moving Group
Couture, D., Gagné, J., & Doyon, R. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acb4eb · Cited by 34 · see citing works
“AF Psc:With updated kinematics, this triple star system with separations of 19″ and 1000″ (Malo et al. 2014b; Kraus et al. 2014; Miret-Roig et al. 2020) is a poor kinematic match to the BANYANΣ model of βPMG.”
MethodBowler, B. P., Shkolnik, E. L., Liu, M. C., Schlieder, J. E., Mann, A. W., Dupuy, T. J., Hinkley, S., Crepp, J. R., Johnson, J. A., Howard, A. W., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/806/1/62 · Cited by 33 · see citing works
“Kraus et al. (2014b) also identify it as a candidate Tuc-Hor member, though their measured RV (10.1 ± 0.6 km s−1) disagrees with the expected value assuming group membership by 5.2 km s−1.”
BackgroundInfluentialSelf-citationElliott, P., & Bayo, A. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw926 · Cited by 33 · see citing works
“The BPMG sample is far from complete and there are likely still many lower-mass members to be identified (similar to the Tuc-Hor moving group, see Kraus et al. 2014).”
BackgroundNEW DEBRIS DISKS IN NEARBY YOUNG MOVING GROUPS* †
Moór, A., Kóspál, Á., Ábrahám, P., Balog, Z., Csengeri, T., Henning, T. K., Juhász, A., & Kiss, C. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/826/2/123 · Cited by 33 · see citing works
Winters, J. G., Sevrinsky, R. A., Jao, W., Henry, T. J., Riedel, A. R., Subasavage, J. P., Lurie, J. C., Ianna, P. A., & Finch, C. T. (2016) · The Astronomical Journal · doi:10.3847/1538-3881/153/1/14 · Cited by 33 · see citing works
“%) member of the ∼45 Myr-old (Kraus et al. 2014; Bell et al. 2015) Tucana-Horologium moving group; SCR 0724-3125 low-probability member of the ∼200 Myr old Carina-Near moving group (Zuckerman et al. 2006), with a probability of 28%; SCR 1901-3106 and SCR 2025-1534 as low- and moderate-probability members of the ∼130-1…”
BackgroundHAZMAT. II. Ultraviolet Variability of Low-mass Stars in the GALEX Archive
Miles, B., & Shkolnik, E. L. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa71ab · Cited by 33 · see citing works
Self-citationAge Spreads and the Temperature Dependence of Age Estimates in Upper Sco
方其, Q. 亮. F., 沈雷, G. J. 歌. H., & Rizzuto, A. C. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa74ca · Cited by 33 · see citing works
“In the magnetic Feiden models, the inferred ages of a 4200 K low mass star are 40 Myr in the Beta Pic Moving Group and 50 Myr in the Tuc-Hor Association, older than the respective Lithium depletion boundary ages of ∼ 24 and 40 Myr (Binks and Jeffries 2014; Malo et al. 2014; Kraus et al. 2014).”
BackgroundCrundall, T. D., Ireland, M., Krumholz, M. R., Federrath, C., Žerjal, M., & Hansen, J. T. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2376 · Cited by 33 · see citing works
Newton, E. R., Mann, A., Tofflemire, B., Pearce, L., Rizzuto, A., Vanderburg, A. M., Martinez, R., Wang, J., Ruffio, J.-B., Kraus, A., et al. (2019) · Keele Research Repository (Keele University) · Cited by 32 · see citing works
Self-citationEstimating the Ultraviolet Emission of M Dwarfs with Exoplanets from Ca ii and Hα
Melbourne, K., Youngblood, A., France, K., Froning, C., Pineda, J., Shkolnik, E., Wilson, D. J., Wood, B., Basu, S., Roberge, A., et al. (2020) · Astronomical Journal · doi:10.3847/1538-3881/abbf5c · Cited by 26 · see citing works
Self-citationA WISE-based search for debris discs amongst M dwarfs in nearby, young, moving groups
Binks, A. S., & Jeffries, R. D. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx838 · Cited by 31 · see citing works
Kerr, R. M. P., Kraus, A. L., Murphy, S. J., Krolikowski, D. M., Bedding, T. R., & Rizzuto, A. C. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/aca0dd · Cited by 31 · see citing works
“…our ability to resolve differences between sequences is considerably weakened by the lack of Li measurements for stars with 1.2 < GBP − GRP < 2.0 where these abundances change most quickly for this age range, with the exception of Tuc-Hor, which has much deeper coverage through Kraus et al. (2014).”
BackgroundMethodResultInfluentialSelf-citationA nearby young M dwarf with a wide, possibly planetary-mass companion
Deacon, N., Schlieder, J., & Murphy, S. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw172 · Cited by 27 · see citing works
“We first constructed a list of known and candidate young stars in nearby young moving groups from Torres et al. (2008), Shkolnik et al. (2009), Schlieder et al. (2012), Kraus et al. (2014) and Malo et al. (2014).”
BackgroundMethodHAZMAT. VII. The Evolution of Ultraviolet Emission with Age and Rotation for Early M Dwarf Stars
Loyd, R. O. P., Shkolnik, E. L., Schneider, A. C., Richey-Yowell, T., Jackman, J. A. G., Peacock, S., Barman, T., Pagano, I., & Meadows, V. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abd0f0 · Cited by 29 · see citing works
Self-citation
- 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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