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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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“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).”
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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).”
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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
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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
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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-citationTHE HAWAII INFRARED PARALLAX PROGRAM. II. YOUNG ULTRACOOL FIELD DWARFS* †
Liu, M. C., Dupuy, T. J., & Allers, K. (2016) · The Astrophysical Journal · doi:10.3847/1538-4357/833/1/96 · Cited by 245
“…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
“…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
“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
“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 175
“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
“…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 165
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
“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
“…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
“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
“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
“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
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
“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
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
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
“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
Krolikowski, D. M., Kraus, A. L., & Rizzuto, A. C. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/ac0632 · Cited by 98
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
“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
“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
“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
“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 99
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
“…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
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
“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
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
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
“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
“…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
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 76
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
“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 69
“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
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
“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
“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 63
“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 63
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
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
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
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
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
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 61
“…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
Binks, A. S., & Jeffries, R. D. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2431 · Cited by 54
“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
“…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
“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
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 56
“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
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
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 54
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
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
“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
“…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
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
“…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
“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
“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
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
“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
“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
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
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
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
“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
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
“…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
“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
“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
Self-citationWood, M. L., Mann, A. W., Barber, M. G., Bush, J. L., Kraus, A. L., Tofflemire, B. M., Vanderburg, A. M., Newton, E. R., Feiden, G. A., Zhou, G., et al. (2023) · The Astronomical Journal · doi:10.3847/1538-3881/aca8fc · Cited by 43
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
“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
“…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
“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
“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
“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 38
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
“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 35
“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
“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
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
“%) 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
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
“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
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
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
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
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
“…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
“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
Self-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
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
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