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A Moving Cluster Distance to the Exoplanet 2M1207b in the TW Hydrae Association
Open accessAbstract
A candidate extrasolar planet companion to the young brown dwarf 2MASSW J1207334-393254 (hereafter 2M1207) was recently discovered by Chauvin et al. They find that the temperature and luminosity of 2M1207b are consistent with a young, ~5 M J planet. The 2M1207 system is purported to be a member of the TW Hya association (TWA) and situated ~70 pc away. Using a revised space motion vector for TWA and improved proper motion for 2M1207, I use the moving cluster method to estimate the distance to the 2M1207 system and other TWA members. The derived distance for 2M1207 (53 ± 6 pc) forces the brown dwarf and planet to be half as luminous as previously thought. The inferred masses for 2M1207A and 2M1207b decrease to ~21 and ~3-4 M J , respectively, with the mass of 2M1207b well below the observed tip of the planetary mass function and the theoretical deuterium-burning limit. After removing probable Lower Centaurus Crux (LCC) members from the TWA sample, as well as the probable nonmember TWA 22, the remaining TWA membership is found to have distances of 49 ± 3 (s.e.m.) ± 12 (1 σ) pc and an internal one-dimensional velocity dispersion of 0.8 km s -1 . There is weak evidence that the TWA is expanding, and the data are consistent with a lower limit on the expansion age of 10 Myr (95% confidence).
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Cites
Monet, D. G., Levine, S. E., Canzian, B., Ables, H. D., Bird, A. R., Dahn, C. C., Guetter, H. H., Harris, H. C., Henden, A. A., Leggett, S. K., et al. (2003) · The Astronomical Journal · doi:10.1086/345888 · Cited by 2,203
Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458
Baraffe, I., Chabrier, G., Barman, T., Allard, F. C., & Hauschildt, P. H. (2003) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361:20030252/pdf · Cited by 1,617
Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458
Baraffe, I., Chabrier, G., Barman, T. S., Allard, F. C., & Hauschildt, P. H. (2003) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20030252 · Cited by 1,493 · cited 1×
“Using the constraints on luminosity and age (Chauvin et al. 2005), I interpolate masses from the non-gray evolutionary tracks of Burrows et al. (1997), the DUSTY tracks of Chabrier et al. (2000), and the COND tracks of Baraffe et al. (2003).”
MethodA Nongray Theory of Extrasolar Giant Planets and Brown Dwarfs
Burrows, A. S., Marley, M. S., Hubbard, W. B., Lunine, J. I., Guillot, T., Saumon, D., Freedman, R., Sudarsky, D., & Sharp, C. M. (1997) · The Astrophysical Journal · doi:10.1086/305002 · Cited by 1,371 · cited 2×
“For all three models, the inferred upper mass limit of 2M1207 B (∼5-7MJup) is less than half of the deuterium-burning mass limit (∼13MJup; Burrows et al. 1997), and less than half of the maximum mass of Doppler velocity planets (∼15MJup; Marcy et al. 2005).”
BackgroundMethodA [ITAL]Hipparcos[/ITAL] Census of the Nearby OB Associations
de Zeeuw, P. T., Hoogerwerf, R., de Bruijne, J. H. J., Brown, A. G. A., & Blaauw, A. (1999) · The Astronomical Journal · doi:10.1086/300682 · Cited by 1,317
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Press, W. H., Teukolsky, S. A., Vetterling, W. T., & Flannery, B. P. (1992) · Cambridge University Press eBooks · Cited by 1,156
Evolutionary Models for Very Low-Mass Stars and Brown Dwarfs with Dusty Atmospheres
Chabrier, G., Baraffe, I., Allard, F., & Hauschildt, P. (2000) · The Astrophysical Journal · doi:10.1086/309513 · Cited by 1,057 · cited 1×
“Using the constraints on luminosity and age (Chauvin et al. 2005), I interpolate masses from the non-gray evolutionary tracks of Burrows et al. (1997), the DUSTY tracks of Chabrier et al. (2000), and the COND tracks of Baraffe et al. (2003).”
MethodA giant planet candidate near a young brown dwarf
Chauvin, G., Lagrange, A. ‐., Dumas, C., Zuckerman, B., Mouillet, D., Song, I., Beuzit, J.-L., & Lowrance, P. (2004) · Astronomy and Astrophysics · doi:10.1051/0004-6361:200400056 · Cited by 686 · cited 6×
“With the previous distance estimates (∼70 pc), Chauvin et al. (2004) estimates mass of 25MJup and 5MJup for A and B, respectively.”
BackgroundMethodInfluentialDetection of Thermal Emission from an Extrasolar Planet
Charbonneau, D., Allen, L. E., Megeath, S. T., Torres, G., Alonso, R., Brown, T. M., Gilliland, R. L., Latham, D. W., Mandushev, G., O’Donovan, F. T., et al. (2005) · The Astrophysical Journal · doi:10.1086/429991 · Cited by 644 · cited 1×
“None have been directly imaged, however two have had their light detected through transit studies with the Spitzer Space Telescope (HD 209458b and TRes-1b; Charbonneau et al. 2005; Deming et al. 2005).”
BackgroundThe Second US Naval Observatory CCD Astrograph Catalog (UCAC2)
Zacharias, N., Urban, S. E., Zacharias, M. I., Wycoff, G. L., Hall, D. M., Monet, D. G., & Rafferty, T. J. (2004) · The Astronomical Journal · doi:10.1086/386353 · Cited by 616
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Cited by
Sorted by citations
Items 101–200 of 231
The chemistry of disks around T Tauri and Herbig Ae/Be stars
Agúndez, M., Roueff, E., Petit, F. L., & Bourlot, J. L. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201732518 · Cited by 60
“The intrinsic stellar brightness is calculated adopting a distance to the star of 51 pc (Mamajek 2005), a stellar radius of 1 R (Webb et al. 1999), and a negligible interstellar reddening (Bergin et al. 2003).”
MethodStelzer, B., Scholz, A., & Jayawardhana, R. (2007) · The Astrophysical Journal · doi:10.1086/521431 · Cited by 61
“Mamajek (2005) has revised the previous distance estimate of 2M 1207 using the moving cluster method, resulting in 53 6 pc. 2M 1207 is the oldest brown dwarf known to actively accrete from a disk, and thus represents a benchmark in constraining the disk lifetimes in the substellar regime.”
MethodLOW EXTREME-ULTRAVIOLET LUMINOSITIES IMPINGING ON PROTOPLANETARY DISKS
Pascucci, I., Ricci, L., Gorti, U., Hollenbach, D. J., Hendler, N. P., Brooks, K., & Contreras, Y. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/795/1/1 · Cited by 61
The Trigonometric Parallax of the Brown Dwarf Planetary System 2MASSW J1207334-393254
Gizis, J. E., Jao, W., Subasavage, J. P., & Henry, T. J. (2007) · The Astrophysical Journal · doi:10.1086/523271 · Cited by 60
“The position angle expected for motion towards Mamajek (2005)’s TWA convergent point is 251.4 degrees, consistent with the measured proper motion.”
BackgroundMethodInfluentialPerryman, M. A. C. (2011) · Cambridge University Press eBooks · doi:10.1017/cbo9780511994852.011 · Cited by 71
Scattered light shadows in warped protoplanetary discs
Nealon, R., Pinte, C., Alexander, R. D., Mentiplay, D., & Dipierro, G. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz346 · Cited by 60
“Such an asymmetry is difficult to explain as TW Hya is considered to be an isolated, single star system (Mamajek 2005; Gagné et al. 2017)— broadly ruling out interactions with external perturbers or the interaction of the disc with © 2015 The Authors ar X iv :1 90 2.”
BackgroundSSSPM J1102-3431 brown dwarf characterization from accurate proper motion and trigonometric parallax
Teixeira, R., Ducourant, C., Chauvin, G., Krone-Martins, A., Song, I., & Zuckerman, B. (2008) · Astronomy and Astrophysics · doi:10.1051/0004-6361:200810133 · Cited by 59
“Considering SSSPM J1102 as a member of TWA, from our astrometric measurements and the convergent point from Mamajek 2005, we can estimate the SSSPM J1102 radial velocity Vr = 14.13 ± 0.79 km s−1 leading to the spacial velocity components: (−11.4, −19.3, −4.7) km s−1, very similar to that of TW…”
MethodInfluentialDisks and outflows in CO rovibrational emission from embedded, low-mass young stellar objects
Herczeg, G. J., Brown, J. M., van Dishoeck, E. F., & Pontoppidan, K. M. (2011) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201016246 · Cited by 58
“TW Hya is an∼ 8 Myr star (Mamajek, 2005) with a disk that has an inner dust hole of∼ 4 AU (Calvet et al., 2002) and an accretion rate of∼ 1.5 × 10−9 M⊙ yr−1 (Herczeg & Hillenbrand, 2008).”
BackgroundInfluentialBiller, B. A., & Close, L. M. (2007) · The Astrophysical Journal · doi:10.1086/523799 · Cited by 57
“Mamajek (2005) estimates a theoretical moving cluster distance to 2M1207 of 53±6 pc and infers masses for 2M1207A and b (with an age of 8 Myr) of ∼21 MJup and ∼3-4 MJup respectively.”
BackgroundThe TEXES Survey for H2Emission from Protoplanetary Disks
Bitner, M. A., Richter, M. J., Lacy, J. H., Herczeg, G. J., Greathouse, T. K., Jaffe, D. T., Salyk, C., Blake, G. A., Hollenbach, D. J., Doppmann, G. W., et al. (2008) · The Astrophysical Journal · doi:10.1086/592317 · Cited by 57
Analysis 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
TW HYA ASSOCIATION MEMBERSHIP AND NEWWISE-DETECTED CIRCUMSTELLAR DISKS
Schneider, A., Melis, C., & Song, I. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/754/1/39 · Cited by 54
“The disk fraction for TWA was again estimated in Looper et al. (2010a), using the list of members from Mamajek (2005).”
MethodTsuboi, Y., Yamazaki, K., Sugawara, Y., Kawagoe, A., Kaneto, S., Iizuka, R., Matsumura, T., Nakahira, S., Higa, M., Matsuoka, M., et al. (2016) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psw081 · Cited by 54
A Number of nearby Moving Groups May Be Fragments of Dissolving Open Clusters
Gagné, J., Faherty, J. K., Moranta, L., & Popinchalk, M. (2021) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ac0e9a · Cited by 53
“Such studies typically worked directly in sky coordinates and proper motion space (Mamajek 2005) or used Bayesian model selection methods to capture the missing low-mass members (Malo et al. 2013; Gagné et al. 2018b).”
MethodSTRINGENT LIMITS ON THE POLARIZED SUBMILLIMETER EMISSION FROM PROTOPLANETARY DISKS
Hughes, A. M., Wilner, D. J., Cho, J., Marrone, D. P., Lazarian, A., Andrews, S. M., & Rao, R. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/704/2/1204 · Cited by 53
“TW Hya is a K star located at a distance of only 51 pc (Mamajek 2005; Hoff et al. 1998).”
BackgroundFirst High‐Contrast Science with an Integral Field Spectrograph: The Substellar Companion to GQ Lupi
McElwain, M. W., Metchev, S., Larkin, J. E., Barczys, M., Iserlohe, C., Krabbe, A., Quirrenbach, A., Weiss, J. L., & Wright, S. A. (2007) · The Astrophysical Journal · doi:10.1086/510063 · Cited by 51
“An age >10 Myr can be excluded if we treat GQ Lup A as a classical T Tauri star which are not typically found in associations older than ∼10 Myr (the approximate age of the TW Hya association; Kastner et al. 1997; Mamajek 2005).”
MethodDynamical Evolution of the TW Hydrae Association
Reza, R. D. L., Jilinski, E. G., & Ortega, V. G. (2006) · The Astronomical Journal · doi:10.1086/501525 · Cited by 51
A kinematic study and membership analysis of the Lupus star-forming region
Galli, P. A. B., Bertout, C., Teixeira, R., & Ducourant, C. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201220704 · Cited by 50
“This was done, for example, for the TW Hydrae association by Mamajek (2005) and for the Taurus-Auriga SFR by Bertout & Genova (2006).”
BackgroundMethodYoung stars inϵChamaleontis and their disks: disk evolution in sparse associations
Fang, M., van Boekel, R., Bouwman, J., Henning, T. K., Lawson, W. A., & Sicilia‐Aguilar, A. (2012) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201118528 · Cited by 50
“Our catalog is based on the TW Hya membership criteria as refined by Mamajek (2005), and includes TWA-1, 2A, 2B, 3A, 3B, 4, 5A, 5B, 6, 7, 8A, 8B, 9A, 9B, 10, 11A, 11B, 13A, 13B, 14, 15A, 15B, 16, 20, 21, 23, 25, 26, 27, 28, plus new identified members TWA-29 30A, 30B (Looper et al. 2007, 2010a,b).”
Using Ice and Dust Lines to Constrain the Surface Densities of Protoplanetary Disks
Powell, D., Murray-Clay, R., & Schlichting, H. E. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa6d7c · Cited by 49
“These error bars are slightly larger than those derived from treating the systematic uncertainty in distance to the TW Hya system alone ( = d 54 6 pc or = d 51 6 pc Mamajek 2005; van Leeuwen 2007, which gives uncertainties that roughly range from±3 au at l = 9 mmobs to±7 au at l = 0.87 mmobs ).”
BackgroundInfluentialA resolved molecular gas disk around the nearby a star 49 Ceti
Hughes, A. M., Wilner, D. J., Kamp, I., & Hogerheijde, M. R. (2008) · University of Groningen research database (University of Groningen / Centre for Information Technology) · Cited by 49
NEW PARALLAXES AND A CONVERGENCE ANALYSIS FOR THE TW Hya ASSOCIATION
Donaldson, J. K., Weinberger, A. J., Gagné, J., Faherty, J. K., Boss, A. P., & Keiser, S. A. (2016) · The Astrophysical Journal · doi:10.3847/1538-4357/833/1/95 · Cited by 48
“In position, the groups are more separated, but some proposed TWA members appear more closely associated with LCC. Mamajek (2005) describes the marker between where TWA ends and LCC begins as a distance of 85 pc.”
BackgroundInfluentialIDENTIFYING NEARBY, YOUNG, LATE-TYPE STARS BY MEANS OF THEIR CIRCUMSTELLAR DISKS
Schneider, A., Song, I., Melis, C., Zuckerman, B., & Bessell, M. S. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/757/2/163 · Cited by 46
“We also estimate the kinematic distance by obtaining a kinematic parallax following the method described in Mamajek (2005).”
MethodTHE COOLEST ISOLATED BROWN DWARF CANDIDATE MEMBER OF TWA
Gagn'e, J., Faherty, J., Cruz, K., Lafrèniere, D., Doyon, R., Malo, L., & Artigau, É. (2014) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/785/1/l14 · Cited by 27
“5 candidate; see Mamajek 2005 and Looper et al. 2007) to confirm our results.”
ResultWISE 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
“Adopting the Malo et al. (2014a) mean space motion for Carina and our new proper motion for WISE J0808−6443, we use the convergent point method (e.g. Mamajek 2005) to calculate a kinematic parallax ($kin = 11.16± 1.13 mas; d = 90± 9 pc) and predicted radial velocity (21.5± 1.2 km s−1).”
MethodInfluentialSelf-citationZhang, Z.-J., Liu, M. C., Best, W., Dupuy, T., & Siverd, R. (2021) · Astrophysical Journal · doi:10.3847/1538-4357/abe3fa · Cited by 35
“…has been made to identify new members of nearby YMGs and has spawned a variety of methods for membership assessment (e.g., Zuckerman et al. 2004; Mamajek 2005; Torres et al. 2006; Shkolnik et al. 2012; Malo et al. 2013; Bowler et al. 2017, 2019; Riedel et al. 2017; Gagné et al. 2018b; Crundall…”
MethodA WIDELY SEPARATED, HIGHLY OCCLUDED COMPANION TO THE NEARBY LOW-MASS T TAURI STAR TWA 30Preprint
Looper, D. L., Bochanski, J. J., Burgasser, A. J., Mohanty, S., Mamajek, E. E., Faherty, J. K., West, A. A., & Pitts, M. A. (2010) · DSpace@MIT (Massachusetts Institute of Technology) · Cited by 44
Self-citationA 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
“We plotted the members of the TWA as if they were located at the d = 97 pc distance to the η Cha cluster (see Mamajek 2005 for kinematic distances to the TWA members).”
BackgroundMethodInfluentialJWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B*
Luhman, K. L., Tremblin, P., Birkmann, S. M., Manjavacas, E., Valenti, J. A., de Oliveira, C. A., Beck, T. L., Giardino, G., Lützgendorf, N., Rauscher, B. J., et al. (2023) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/acd635 · Cited by 43
“They then derived a mass by comparing the luminosity to the values predicted by evolutionary models for the age of TWA (Chauvin et al. 2004; Mamajek 2005; Mamajek & Meyer 2007; Ducourant et al. 2008; Barman et al. 2011b).”
MethodMcJunkin, M., France, K., Schneider, P. C., Herczeg, G. J., Brown, A., Hillenbrand, L., Schindhelm, R., & Edwards, S. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/780/2/150 · Cited by 42
Kinematic analysis and membership status of TWA22 AB
Teixeira, R., Ducourant, C., Chauvin, G., Krone-Martins, A., Bonnefoy, M., & Song, I. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200912173 · Cited by 42
“Their radial velocities were extracted from Table 1 of Mamajek (2005) (Torres et al. 2003 data for TWA 01 and TWA9A; Torres et al. 1995 for TWA4; Reid 2003 for TWA11; and Mohanty et al. 2003 for 2M1207A).”
BackgroundMethodTofflemire, B. M., Mathieu, R. D., & Johns‐Krull, C. M. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab4f7d · Cited by 41
“…following is a summary of the study by Kellogg et al. (2017), where we highlight their results for the inner binary, TWA 3A. TWA 3 is a member of the ∼10 Myr TW Hya association (Mamajek 2005), composed of an inner spectroscopic binary, TWA 3A, and an outer triple companion, TWA 3B, separated by 1.”
BackgroundTsuboi, Y., Tsuboi, Y., Yamazaki, K., Yamazaki, K., Sugawara, Y., Sugawara, Y., Kawagoe, A., Kawagoe, A., Kaneto, S., Kaneto, S., et al. (2016) · Institutional Repositories DataBase (IRDB) · Cited by 41
Measuring the Mass of a Pre-Main-Sequence Binary Star through the Orbit of TWA 5A
Konopacky, Q., Ghez, A. M., Duchêne, G., McCabe, C., & Macintosh, B. (2007) · The Astronomical Journal · doi:10.1086/513010 · Cited by 41
“Additionally, TW Hydrae is quite nearby, with an average distance of ∼50 pc (e.g., Makarov & Fabricius 2001, Mamajek 2005).”
A Census of the TW Hya Association with Gaia*
Luhman, K. L. (2023) · The Astronomical Journal · doi:10.3847/1538-3881/accf19 · Cited by 40
“Previous studies have attempted to derive both ages for TWA (Makarov et al. 2005; Mamajek 2005; de la Reza et al. 2006; Ducourant et al. 2014; Donaldson et al. 2016).”
BackgroundTHE NEAREST ISOLATED MEMBER OF THE TW HYDRAE ASSOCIATION IS A GIANT PLANET ANALOG
Kellogg, K., Metchev, S., Gagné, J., & Faherty, J. K. (2016) · The Astrophysical Journal Letters · doi:10.3847/2041-8205/821/1/l15 · 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
“…that can assign membership probabilities with missing parts of the six-dimensional space and velocity, including the convergent point method (Mamajek 2005; Torres et al. 2006) and various other flavors of selection cuts in space velocity and/or photometry (Zuckerman & Song 2004; Kraus et…”
MethodSelf-citationMorrow, A. L., Luhman, K. L., Espaillat, C. C., D’Alessio, P., Adame, L., Calvet, N., Forrest, W. J., Sargent, B., Hartmann, L. W., Watson, D. M., et al. (2008) · The Astrophysical Journal · doi:10.1086/587462 · Cited by 39
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
“Prior to the determination of a parallax from Gaia DR2, we used the methodology of Mamajek (2005), the UCAC5 (Zacharias et al. 2017) proper motion for EPIC 247267267, and the “spaghetti” velocity solution from de Zeeuw et al. (1999), to find the bulk of EPIC 247267267’s proper motion appeared to be…”
MethodSelf-citationDesidera, S., Covino, E., Messina, S., Carson, J., Hagelberg, J., Schlieder, J. E., Biazzo, K., Alcalá, J. M., Chauvin, G., Vigan, A., et al. (2014) · arXiv (Cornell University) · doi:10.48550/arxiv.1405.1559 · Cited by 37
L and T dwarfs in the Hyades and Ursa Major moving groups
Bannister, N. P., & Jameson, R. F. (2007) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1111/j.1745-3933.2007.00312.x · Cited by 32
A 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
“Target L, 2MASSJ12073346-3932539 - Literature searches for any additional evidence for a disc revealed that this target was the brown dwarf 2M1207, which is host to the giant exoplanet candidate 2M1207b (Mamajek 2005; Barman et al. 2011).”
BackgroundPascucci, I., Edwards, S., Heyer, M., Rigliaco, E., Hillenbrand, L., Gorti, U., Hollenbach, D., & Simon, M. N. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/814/1/14 · Cited by 31
“This conclusion is also consistent with the lack of absorption in the Na I and K I profiles of TW Hya, which is at only ∼50 pc from the Sun (Mamajek 2005), albeit in a different direction from Taurus.”
ResultCaballero, J. A. (2018) · Geosciences · doi:10.3390/geosciences8100362 · Cited by 31
The Trigonometric Parallax of the Brown Dwarf Planetary System 2MASSW J1207334-393254Preprint
Gizis, J. E., Jao, W., Subasavage, J. P., & Henry, T. J. (2012) · Cited by 30
ALMA Observations of the Young Substellar Binary System 2M1207
Ricci, L., Cazzoletti, P., Czekala, I., Andrews, S. M., Wilner, D. J., Szücs, L., Lodato, G., Testi, L., Pascucci, I., Mohanty, S., et al. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa78a0 · Cited by 29
“The uncertainty of these mass estimates is typically reported as ≈ 3 MJup and is dominated by the assumptions on the formation pathway and accretion history (see discussions in Mamajek 2005; Bowler 2016, Section 3).”
BackgroundResultM STARS IN THE TW HYA ASSOCIATION: STELLAR X-RAYS AND DISK DISSIPATION
Kastner, J. H., Principe, D. A., Punzi, K., Stelzer, B., Gorti, U., Pascucci, I., & Argiroffi, C. (2016) · The Astronomical Journal · doi:10.3847/0004-6256/152/1/3 · Cited by 28
“TWA 22: Mamajek (2005) finds a low probability that TWA 22 (M5) is a TWA member; Teixeira et al. (2009) concluded this star is a member of the β Pic Moving Group (rather than the TWA); and Ducourant et al. (2014) find that TWA 22 fails their convergence point membership analysis.”
BackgroundA Pre-Gaia Census of Nearby Stellar Groups
Mamajek, E. E. (2015) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921315006250 · Cited by 28
“The ∼10 Myr-old TW Hya association is a well-characterized group of ∼3 dozen stars (Kastner et al. 1997, Mamajek 2005, Weinberger et al. 2013, Ducourant et al. 2014), and will not be discussed further.”
BackgroundSelf-citationPicos, D. G., Snellen, I. A. G., de Regt, S., Landman, R., Zhang, Y., Gandhi, S., Ginski, C., Kesseli, A. Y., Mollière, P., & Stolker, T. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202450028 · Cited by 26
A revised moving cluster distance to the Pleiades open cluster
Galli, P. A. B., Moraux, E., Bouy, H., Bouvier, J., Olivares, J., & Teixeira, R. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201629239 · Cited by 26
“In the following, we apply the CPSM to the TW Hydrae association whose CP position is well established (Mamajek 2005; Ducourant et al. 2014) to calibrate our new implementation of the CPSM and illustrate its application.”
BackgroundMethodSignatures of warm carbon monoxide in protoplanetary discs observed with Herschel SPIRE★
van der Wiel, M. H. D., Naylor, D. A., Kamp, I., Ménard, F., Thi, W. ‐., Woitke, P., Olofsson, G., Pontoppidan, K. M., Francesco, J. D., Glauser, A. M., et al. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1462 · Cited by 24
A revised moving cluster distance to the Pleiades open cluster
Galli, P. A. B., Moraux, E., Bouy, H., Bouvier, J., Olivares, J., & Teixeira, R. (2017) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201629239/pdf · Cited by 24
The TWA 3 Young Triple System: Orbits, Disks, Evolution
Kellogg, K., Prato, L. A., Torres, G., Schaefer, G. H., Avilez, I., Ruiz-Rodriguez, D. A., Wasserman, L. H., Bonanos, A. Z., Guenther, E. W., Neuhäuser, R., et al. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa7c60 · Cited by 24
“Adopting a value for the angular semimajor axis, 5.6mas, that falls in the average of the range of well-defined confidence intervals, 4.7–6.5 mas, and assuming a distance of 34 pc (Mamajek 2005), we estimate the physical size of the semimajor axis to be ∼0.19au.”
BackgroundMethodInfluentialAsensio-Torres, R., Currie, T., Janson, M., Desidera, S., Kuzuhara, M., Hodapp, K. W., Brandt, T. D., Guyon, O., Lozi, J., Groff, T., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201834688 · Cited by 24
“TWA is located at ∼50 pc and, like USco, it has an estimated age of ∼10 Myr (Webb et al. 1999; Mamajek 2005; Donaldson et al. 2016).”
BackgroundThe enigmatic young brown dwarf binary FU Tau: accretion and activity
Stelzer, B., Scholz, A., Argiroffi, C., & Micela, G. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.17182.x · Cited by 23
The young, tight, and low-mass binary TWA22AB: a new calibrator for evolutionary models?
Bonnefoy, M., Chauvin, G., Dumas, C., Lagrange, A. ‐., Beust, H., Desort, M., Teixeira, R., Ducourant, C., Beuzit, J.-L., & Song, I. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200810921 · Cited by 38
“Later, Mamajek (2005) question the membership of TWA22 from a kinematic study of TW Hydrae members.”
BackgroundInfluentialRadio Constraints on Activity in Young Brown Dwarfs
Osten, R. A., & Jayawardhana, R. (2006) · The Astrophysical Journal · doi:10.1086/505328 · Cited by 22
“Mamajek (2005) used the moving cluster method to estimate a distance of 43±7 pc to this object.”
MethodKINEMATICS OF IONIZED GAS AT 0.01 AU OF TW Hya
Goto, M., Carmona, A., Linz, H., Stecklum, B., Henning, T. K., Meeus, G., & Usuda, T. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/748/1/6 · Cited by 22
“Close vicinity of TW Hya to the solar system (50–60 pc; Kastner et al. 1997; Hoff, Henning, & Pfau 1998; Mamajek 2005) makes it an exceptional laboratory to look into the central few AU of a disk (we will use d =51 pc from Mamajek (2005) throughout this paper).”
BackgroundManjavacas, E., Tremblin, P., Birkmann, S. M., Valenti, J. A., de Oliveira, C. A., Beck, T. L., Giardino, G., Lützgendorf, N., Rauscher, B. J., & Marco Sirianni, A. (2024) · The Astronomical Journal · doi:10.3847/1538-3881/ad2938 · Cited by 23
Spectral library of age-benchmark low-mass stars and brown dwarfs
Manjavacas, E., Lodieu, N., Béjar, V. J. S., Osorio, M. R. Z., Boudreault, S., & Bonnefoy, M. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz3441 · Cited by 21
“…objects from α Persei (90±10 Myr; Stauffer et al. 1999; Barrado y Navascués 2004), seven objects from Rho Ophiuchi (0.3+2.7−0.2 Myr; Wilking et al. 2005), two of TWA (10±3 Myr; Mamajek 2005), 13 objects from Taurus (1.5±0.5 Myr; Briceño et al. 2002), and 12 from the UppSco association (5−10 Myr).”
BackgroundInfluentialUsing Ice and Dust Lines to Constrain the Surface Densities of Protoplanetary Disks
Powell, D., Murray-Clay, R. A., & Schlichting, H. E. (2017) · DSpace@MIT (Massachusetts Institute of Technology) · Cited by 21
New binaries from the SHINE survey
Bonavita, M., Gratton, R., Desidera, S., Squicciarini, V., D’Orazi, V., Zurlo, A., Biller, B. A., Chauvin, G., Fontanive, C., Janson, M., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202140510 · Cited by 21
A FORMATION SCENARIO OF YOUNG STELLAR GROUPS IN THE REGION OF THE SCORPIO CENTAURUS OB ASSOCIATION
Ortega, V. G., Jilinski, E., de la Reza, R., & Bazzanella, B. (2009) · The Astronomical Journal · doi:10.1088/0004-6256/137/4/3922 · Cited by 21
“…al. 1999, Zuckerman et al. 2001, Ortega et al. 2002, 2004), TW Hydrae (TWA) (de la Reza et al. 1989, Kastner et al. 1997, Webb et al. 1999, Reid 2003, Mamajek 2005, de la Reza et al. 2006) and the compact young cluster η Chamaeleontis (η Cha) (Mamajek et al. 1999, 2000, Jilinski et al. 2005) are…”
BackgroundThe age rank of the nearest pre-main-sequence groups
Lawson, W. A., Lyo, A.-R., & Bessell, M. S. (2009) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1111/j.1745-3933.2009.00755.x · Cited by 21
A new method for calculating the convergent point of a moving group
Galli, P. A. B., Teixeira, R., Ducourant, C., Bertout, C., & Benevides‐Soares, P. (2011) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201118277 · Cited by 21
“These two dynamical states are st ictly equivalent as far as proper motions are concerned and radialvelocity information is needed to distinguish between them (Blaauw 1964). parallaxes are not available (for recent applications of this strategy see Mamajek 2005; Bertout & Genova 2006).”
BackgroundDynamical masses of M-dwarf binaries in young moving groups
Rodet, L., Bonnefoy, M., Durkan, S., Beust, H., Lagrange, A. ‐., Schlieder, J. E., Janson, M., Grandjean, A., Chauvin, G., Messina, S., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201832924 · Cited by 20
Zhang, Z.-J., Mollière, P., Fortney, J., & Marley, M. (2025) · Astronomical Journal · doi:10.3847/1538-3881/addfcb · Cited by 16
Kinematics of the Gould Belt based on open clusters
Bobylev, V. V. (2006) · Astronomy Letters · doi:10.1134/s1063773706120036 · Cited by 18
“We used the latest data for 25 TWA luster stars from Mamajek (2005).”
MethodDoppler images and chromospheric variability of TWA 17
Skelly, M. B., Unruh, Y. C., Barnes, J. R., Lawson, W. A., Donati, J. ‐., & Cameron, A. C. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15411.x · Cited by 18
“An even more distant estimate is given in Mamajek (2005) where the distance to TWA 17 is 163 ± 46 pc.”
BackgroundMethodEarly phases of planet formation in protoplanetary disks
Henning, T. K. (2008) · Physica Scripta · doi:10.1088/0031-8949/2008/t130/014019 · Cited by 18
A formation scenario of young stellar groups in the region of the Scorpio Centaurus OB associationPreprint
Ortega, V. G., Jilinski, E. G., Reza, R. D. L., & Bazzanella, B. (2012) · Cited by 18
L and T dwarfs in the Hyades and Ursa Major moving groups
Bannister, N., & Jameson, R. F. (2007) · Figshare · Cited by 17
Kinematics of the Scorpius-Centaurus OB association
Bobylev, V. V., & Bajkova, A. T. (2007) · Astronomy Letters · doi:10.1134/s1063773707090010 · Cited by 17
“There are both radial velocities and proper motions for some of these stars (Makarov 2003; Mamajek et al. 2002; Mamajek 2005; Torres et al. 2006).”
BackgroundMethodInfluentialKinematics of the Gould Belt Based on Open Clusters
Bobylev, V. V. (2006) · CERN Document Server (European Organization for Nuclear Research) · Cited by 16
Arnold, T. J., Eisner, J. A., Monnier, J. D., & Tuthill, P. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/750/2/119 · Cited by 15
“TW Hydrae (TW Hya), a classical T Tauri Star, is one of the closest transition disks, located in the nearby (∼50 pc; Mamajek 2005) TW Hya Association.”
BackgroundA SURVEY FOR A COEVAL, COMOVING GROUP ASSOCIATED WITH HD 141569
Aarnio, A. N., Weinberger, A. J., Stassun, K. G., Mamajek, E. E., & James, D. J. (2008) · The Astronomical Journal · doi:10.1088/0004-6256/136/6/2483 · Cited by 14
“…(the ratio of one AU in km to a Julian Year in s), μυ is the parallel component of proper motion (proper motion in the direction of the convergent point), v is the velocity of the group in km s−1, and λ is the angular separation between the star and the convergent point (Equation 1, Mamajek 2005).”
BackgroundMethodInfluentialSelf-citationDzib, S. A., Loinard, L., Rodríguez, L. F., & Galli, P. A. B. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/788/2/162 · Cited by 13
“However, this strategy has proven to yield consistent results in young nearby associations (see, e.g., Mamajek 2005; Bertout & Genova 2006) and it will be used in this work only to provide some guidance in our analysis.”
ResultOrbital motion of the young brown dwarf companion TWA 5 B
Neuhäuser, R., Schmidt, T. O. B., Hambaryan, V. V., & Vogt, N. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200913917 · Cited by 14
“Mamajek (2005) reports a kinematical distance of 44± pc for TWA 5, but when using the uncertain TWA 9 parallax estimate in his 2D convergent point method.”
MethodA Large X-Ray Flare from a Single Weak-Lined T Tauri Star TWA-7 Detected with MAXI GSC
Uzawa, A., Tsuboi, Y., Morii, M., Yamazaki, K., Kawai, N., Matsuoka, M., Nakahira, S., Serino, M., Matsumura, T., Mihara, T., et al. (2011) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/63.sp3.s713 · Cited by 12
“The distance to the source is estimated to be 27 ˙ 2 pc by Mamajek (2005) from the moving cluster method (e.g., Atanasijevic 1971; de Bruijne 1999).”
MethodThe surface magnetic activity of the weak-line T Tauri stars TWA 9A and V1095 Sco
Nicholson, B. A., Hussain, G. A. J., Donati, J. ‐., Folsom, C. P., Mengel, M. W., Carter, B. D., & Wright, D. J. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1965 · Cited by 12
“Manara et al. (2013) use the distance of ∼ 68 pc from Mamajek (2005), but assume a different apparent magnitude, and so find a lower luminosity of 0.25 L .”
BackgroundMethodInfluentialDesign Considerations for a Ground-based Search for Transiting Planets around L and T Dwarfs
Tamburo, P., & Muirhead, P. S. (2019) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/ab3a1e · Cited by 12
“A directly-imaged 3-4 MJup companion was discovered at a projected separation of 41 AU around a 25 MJup brown dwarf (Chauvin et al. 2004; Mamajek 2005), and a 0.75 MJup planet was detected at a projected separation of 0.59 AU around a probable brown dwarf in the OGLE-2017-BLG-1522 system by Jung et…”
BackgroundInfluentialThe TW Hydrae Association is a cluster chain of Sco-Cen
Miret-Roig, N., Alves, J., Ratzenböck, S., Galli, P. A. B., Bouy, H., Figueras, F., Großschedl, J. E., Meingast, S., Posch, L., Rottensteiner, A., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202452558 · Cited by 11
Orbital motion of the young brown dwarf companion TWA 5 B
Neuhäuser, R., Schmidt, T. O. B., Hambaryan, V., & Vogt, N. (2009) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/200913917/pdf · Cited by 12
Lee, J., & Song, I. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1044 · Cited by 13
Asensio-Torres, R., Currie, T., Janson, M., Desidera, S., Kuzuhara, M., Hodapp, K. W., Brandt, T. D., Guyon, O., Lozi, J., Groff, T. D., et al. (2019) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201834688/pdf · Cited by 10
PROTOPLANETARY AND TRANSITIONAL DISKS IN THE OPEN STELLAR CLUSTER IC 2395
Balog, Z., Siegler, N., Rieke, G. H., Kiss, L. L., Muzerolle, J., Gutermuth, R. A., Bell, C. P. M., Vinkó, J., Su, K. Y. L., Young, E. T., et al. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/832/1/87 · Cited by 9
“Their existence within a cluster, especially in large numbers, implies stellar ages on the traditional scale of less than about 10 Myr (e.g., Haisch et al. 2001; Hillenbrand 2005; Mamajek 2005).”
BackgroundA SURVEY FOR A COEVAL, COMOVING GROUP ASSOCIATED WITH HD 141569Preprint
Aarnio, A., Weinberger, A. J., Stassun, K. G., Mamajek, E. E., & James, D. J. (2013) · Cited by 9
Self-citationProtoplanetary and Transitional Disks in the Open Stellar Cluster IC 2395
Balog, Z., Siegler, N., Rieke, G. H., Kiss, L. L., Muzerolle, J., & Vinkó, J. (2016) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · Cited by 9
The Solar Neighborhood. XLIII. Discovery of New Nearby Stars with μ < 0.″18 yr−1 (TINYMO Sample)
Riedel, A. R., Silverstein, M. L., Henry, T. J., Jao, W.-C., Winters, J. G., Subasavage, J. P., Malo, L., & Hambly, N. C. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aaca33 · Cited by 8
“…= 9.40, V −Ks = 5.29), is one of the first known members of the TW Hya association (de la Reza et al. 1989), and has for some time been considered the closest genuine member (TWA 22AB, at 17.5±0.2 pc, is now widely believed to be a member of β Pic instead, Mamajek 2005; Teixeira et al. 2009.)”
BackgroundInfluentialKinematics of the Scorpius-Centaurus OB AssociationPreprint
Бобылев, В. В., & Bajkova, A. T. (2012) · Cited by 8
Spectroscopy of Candidate Members of the Sco-Cen Complex*
Luhman, K. L., & Esplin, T. L. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/ac35e4 · Cited by 7
“The Ophiuchus objects are likely to be younger than the association containing TWA 25 and TWA 26 (∼ 10 Myr, Webb et al. 1999; Mamajek 2005), in which case they would have lower surface gravities.”
BackgroundDisentangling disc and atmospheric signatures of young brown dwarfs with JWST/NIRSpec
Picos, D. G., de Regt, S., Gandhi, S., Grasser, N., & Snellen, I. A. G. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202555669 · Cited by 6
ACHANDRAOBSERVATION OF THE TW HYDRAE ASSOCIATION BROWN DWARF 2MASSW J1139511–315921
Castro, P. J., Gizis, J. E., & Gagné, M. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/736/1/67 · Cited by 6
“This association is an ideal place to study BDs and their X-ray emission, with its close proximity of ∼ 50 pc (Mamajek 2005), an age of ∼ 8 − 10 Myr (Song et al. 2003; Webb et al. 1999), and a small sample of well studied bona fide BDs.”
BackgroundThe Isochronal Age Scale of Young Moving Groups in the Solar Neighbourhood
Bell, C. P. M., Mamajek, E. E., & Naylor, T. (2015) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921315006213 · Cited by 5
“…trigonometric parallax measurements, however when this is not an option (or where the parallax estimates appear to be in error or have unusually large uncertainties) we either adopt a kinematic distance from the literature or derive one using the ‘moving cluster’ method (see e.g. Mamajek 2005).”
MethodSelf-citationA New Nearby Candidate Star Cluster in Ophiuchus atd ≃ 170 pc
Mamajek, E. E. (2006) · The Astronomical Journal · doi:10.1086/508205 · Cited by 5
“The convergent point algorithm described in Mamajek (2005) yields a group convergent point of cvp; cvp ’ 117 þ81 19 ; 39 þ24 15 (68% confidence intervals) within a long, narrow ( 1N5wide) error ellipse oriented northwest-southeast.”
BackgroundMethodSelf-citationRX J0942.7−7726AB: an isolated pre-main-sequence wide binary
Murphy, S. J., Lawson, W. A., & Bessell, M. S. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21243.x · Cited by 3
“Mamajek (2005) and Torres et al. (2008) have computed kinematic distances to TWA 16 and TWA 20.”
BackgroundMethodA Herschel PACS survey of brown dwarfs in IC 2391: limits on primordial and debris disc fractions
Riaz, B., & Kennedy, G. M. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1054 · Cited by 3
“4 for the case of the ∼10 Myr old brown dwarf disc 2MASSW J1207334−393254 (2M1207) in the TWA, located at a distance of ∼50 pc (Mamajek 2005).”
BackgroundExoplanet Detection and Its Dependence on Stochastic Sampling of the Stellar Initial Mass Function
Bottrill, A. L., Haigh, M. E., Hole, M. R. A., Theakston, S. C. M., Allen, R. B., Grimmett, L. P., & Parker, R. J. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab8e39 · Cited by 2
“…are in so-called ‘Young Moving Groups’; collections of tens to hundreds of stars of similar ages with coherent proper motion velocities (Zuckerman & Song 2004; Torres et al. 2008; Mamajek 2005; Riedel et al. 2017; Gagné et al. 2018b; Gagné & Faherty 2018; Gagné et al. 2018a; Lee & Song 2019).”
BackgroundExoplanet Detection and Its Dependence on Stochastic Sampling of the Stellar Initial Mass Function
Bottrill, A. L., Haigh, M. E., Hole, M. R. A., Theakston, S. C. M., Allen, R. B., Grimmett, L. P., & Parker, R. J. (2020) · White Rose Research Online (University of Leeds, The University of Sheffield, University of York) · Cited by 2
On the nature of the purported common proper motion companions to the exoplanet host star 51 Peg
Mamajek, E. E. (2010) · Astronomische Nachrichten · doi:10.1002/asna.201011370 · Cited by 1
“I follow the techniques used in Mamajek et al. (2002) and Mamajek (2005) to rotate the equatorial proper motion into components pointed towards the 51 Peg vertex (µυ) and perpendicular (µτ ).”
MethodSelf-citation
Metadata
- Authors
- Mamajek, E. E.
- Affiliations
- Center for Astrophysics Harvard & Smithsonian (US)
- Corresponding author
- Mamajek, Eric E.
- ORCID
- Mamajek, Eric E.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2005-12
- Volume
- 634
- Issue
- 2
- Pages
- 1385-1394
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2063162420
- Cited by
- 232
- References
- 73
- Citations by year
- 2026: 2 · 2025: 4 · 2024: 2 · 2023: 2 · 2022: 1 · 2021: 4 · 2020: 5 · 2019: 7 · 2018: 31 · 2017: 10 · 2016: 13 · 2015: 7 · 2014: 17 · 2013: 14 · 2012: 20
- FWCI
- 9.50
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- CERN Document Server (European Organization for Nuclear Research) (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 › Earth and Planetary Sciences › Space and Planetary Science › Astro and Planetary Science
- Keywords
- TW Hydrae association, brown dwarfs, exoplanets, association membership, velocity dispersion, deuterium burning limit, space motions
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