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MAPPING THE SHORES OF THE BROWN DWARF DESERT. II. MULTIPLE STAR FORMATION IN TAURUS-AURIGA
Open accessAbstract
We have conducted a high-resolution imaging study of the Taurus–Auriga star-forming region in order to characterize the primordial outcome of multiple star formation and the extent of the brown dwarf desert. Our survey identified 16 new binary companions to primary stars with masses of 0.25–2.5 M ☉ , raising the total number of binary pairs (including components of high-order multiples) with separations of 3–5000 AU to 90. We find that ∼2/3–3/4 of all Taurus members are multiple systems of two or more stars, while the other ∼1/4–1/3 appear to have formed as single stars; the distribution of high-order multiplicity suggests that fragmentation into a wide binary has no impact on the subsequent probability that either component will fragment again. The separation distribution for solar-type stars (0.7–2.5 M ☉ ) is nearly log-flat over separations of 3–5000 AU, but lower-mass stars (0.25–0.7 M ☉ ) show a paucity of binary companions with separations of ≳200 AU. Across this full mass range, companion masses are well described with a linear-flat function; all system mass ratios ( q = M B / M A ) are equally probable, apparently including substellar companions. Our results are broadly consistent with the two expected modes of binary formation (free-fall fragmentation on large scales and disk fragmentation on small scales), but the distributions provide some clues as to the epochs at which the companions are likely to form.
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“The multiplicity of class I young stellar objects (YSOs) in embedded clusters and pre-MS stars in young associations is high and ranges from 20% to 60% for the ∼10 1.5 -10 2.5 AU separation range and mass ratios of ∼0.1-1”
From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Kraus et al. 2011
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“The number of binaries is flat in log period or semi-major axis space (Halbwachs et al. 2003;Kraus et al. 2011), and young binaries are similar to field population in this respect (Duchêne et al. 2007).”
From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Kraus et al. 2011
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“However, this is difficult to formulate as binary identifications are not complete at mass ratios less than 0.1 (e.g., Kraus et al. 2011) and the number of secondaries hosting passive disks in the 10 7 year old age range is not well characterized.”
From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Kraus et al. 2011
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Cites
On the Gravitational Stability of a Disk of Stars
Toomre, A. (1964) · The Astrophysical Journal · doi:10.1086/147861 · Cited by 3,349 · cited 2×
“If the disk accumulates material from the envelope more quickly than mass can accrete onto the star, then it could grow more massive and violate the Toomre stability criterion (Toomre 1964), fragmenting to form a bound companion.”
BackgroundA SURVEY OF STELLAR FAMILIES: MULTIPLICITY OF SOLAR-TYPE STARS
Raghavan, D., McAlister, H. A., Henry, T. J., Latham, D. W., Marcy, G. W., Mason, B. D., Gies, D. R., White, R. J., & ten Brummelaar, T. A. (2010) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/190/1/1 · Cited by 1,922
Pre-Main-Sequence Evolution in the Taurus-Auriga Molecular Cloud
Kenyon, S. J., & Hartmann, L. W. (1995) · The Astrophysical Journal Supplement Series · doi:10.1086/192235 · Cited by 1,802
Ghez, A. M., Salim, S., Weinberg, N. N., Lu, J. R., Do, T., Dunn, J. K., Matthews, K., Morris, M. R., Yelda, S., Becklin, E. E., et al. (2008) · The Astrophysical Journal · doi:10.1086/592738 · Cited by 1,577
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
Color Transformations for the 2MASS Second Incremental Data Release
Carpenter, J. M. (2001) · The Astronomical Journal · doi:10.1086/320383 · Cited by 1,090
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
Disk accretion onto magnetic T Tauri stars
Koenigl, A. (1991) · The Astrophysical Journal · doi:10.1086/185972 · Cited by 1,024
Ida, S., & Lin, D. N. C. (2004) · The Astrophysical Journal · doi:10.1086/381724 · Cited by 948
Boyle's Law and Gravitational Instability
Bonnar, W. B. (1956) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/116.3.351 · Cited by 919
Research works printed but not linked: 19
- Baraffe, 1998, A&A, 337, 403
- Bodenheimer, 2001, The Formation of Binary Stars, 13
- Bonnell, 2001, The Formation of Binary Stars, 23
- Bouvier, 1997, A&A, 323, 139
- D'Antona, 1997, Mem. Soc. Astron. Ital., 68, 807
- Duchêne, 1999, A&A, 351, 954
- Duquennoy, 1991, A&A, 248, 485
- Köhler, 2000, A&A, 356, 541
- Königl, 2000, Protostars and Planets IV, 750
- Kraus, 2011, ApJ
- Leinert, 1993, A&A, 278, 129
- Lin, 1985, Protostars and Planets II, 981
- Richichi, 1998, A&A, 330, 578
- Sartoretti, 1998, A&A, 334, 592
- Schmidt-Kaler, 1982, Physical Parameters of the Stars, Landolt-Bornstein Numerical Data and Functional Relationships in Science and Technology, New Series, Group VI, Volume 2b
- Shakura, 1973, A&A, 24, 337
- Shu, 2000, Protostars and Planets IV, 789
- Woitas, 1998, A&A, 338, 122
- Zacharias, 2004, BAAS, 205, 48.15
Cited by
Sorted by citations
Items 101–200 of 324
The properties of discs around planets and brown dwarfs as evidence for disc fragmentation
Stamatellos, D., & Herczeg, G. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv526 · Cited by 37
“There are many brown dwarf companions to Sun-like stars, but these tend to be at wide separations (Kraus et al. 2008, 2011; Faherty et al. 2009, 2010; Evans et al. 2012; Duchêne & Kraus 2013; Reggiani & Meyer 2013).”
BackgroundMAGNETIC ORIGINS OF THE STELLAR MASS-OBLIQUITY CORRELATION IN PLANETARY SYSTEMS
Spalding, C., & Batygin, K. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/811/2/82 · Cited by 65
“On the contrary, binary fraction probably lies somewhere between half and unity during the early, disk-hosting stage of stellar evolution (Ghez et al. 1993; Kraus et al. 2011; Marks & Kroupa 2012; Duchêne & Kraus 2013).”
BackgroundTRANSITIONAL DISKS AND THEIR ORIGINS: AN INFRARED SPECTROSCOPIC SURVEY OF ORION A
Kim, K. H., Watson, D. M., Manoj, P., Forrest, W. J., Najita, J., Furlan, E., Sargent, B. A., Espaillat, C. C., Muzerolle, J. C., Megeath, S. T., et al. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/769/2/149 · Cited by 64
“M⋆ of WTD+PTD. Sensitive searches have been made for 10 AU-scale binaries in Taurus (Pott et al. (2010), Kraus et al. (2011)), but only one (CoKu Tau/4; Ireland & Kraus (2008)) of the nine transitional disk systems so studied has a stellar companion been detected with binary separation similar to…”
MethodSTARSPOT-INDUCED OPTICAL AND INFRARED RADIAL VELOCITY VARIABILITY IN T TAURI STAR HUBBLE I 4
Mahmud, N. I., Crockett, C., Johns‐Krull, C. M., Prato, L. A., Hartigan, P. M., Jaffe, D. T., & Beichman, C. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/736/2/123 · Cited by 64
“Kraus et al. (2011) recently identified Hubble I 4 as a binary using high-resolution imaging, with a separation of 4.1 AU.”
MethodInfluentialTobin, J. J., Dunham, M. M., Looney, L. W., Li, Z.-Y., Chandler, C. J., Segura-Cox, D. M., Sadavoy, S. I., Melis, C., Harris, R. J., Perez, L. M., et al. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/798/1/61 · Cited by 62
“The even higher multiplicity fractions observed in young star forming regions like Taurus suggest that binary formation is commensurate with star formation (Kraus et al. 2011).”
BackgroundSloan Digital Sky Survey. V. Pioneering Panoptic Spectroscopy
Kollmeier, J. A., Rix, H., Aerts, C., Aird, J., Alfaro, P. V., Almeida, A., Anderson, S. F., Arseneau, S., Assef, R. J., Aviram, S., et al. (2025) · The Astronomical Journal · doi:10.3847/1538-3881/ae0576 · Cited by 125
GIARPS High-resolution Observations of T Tauri stars (GHOsT)
Gangi, M. E. M., Antoniucci, S., Biazzo, K., Frasca, A., Nisini, B., Alcalá, J. M., Giannini, T., Manara, C. F., Giunta, A., Harutyunyan, A., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244042 · Cited by 60
Sicilia-Aguilar, A., & Currie, T. (2011) · LA Referencia (Red Federada de Repositorios Institucionales de Publicaciones Científicas) · Cited by 72
ORBITAL MOTION IN PRE-MAIN SEQUENCE BINARIES
Schaefer, G. H., Prato, L. A., Simon, M., & Patience, J. (2014) · The Astronomical Journal · doi:10.1088/0004-6256/147/6/157 · Cited by 59
“The measured separation of the close pair, HV Tau A-B, ranges from 26 to 73 mas (Simon et al. 1992, 1996; Monin & Bouvier 2000; Duchêne et al. 2010; Kraus et al. 2011; this work).”
BackgroundHinkley, S., Kraus, A. L., Ireland, M., Cheetham, A. C., Carpenter, J. M., Tuthill, P., Lacour, S., Evans, T. M., & Haubois, X. (2015) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/806/1/l9 · Cited by 59
“Thus, sensitivity near, and within, the diffraction limit of large telescopes is needed to access smaller orbital separations for Sco-Cen stars (Kraus et al. 2008, 2011).”
BackgroundInfluentialSelf-citationWide binaries are rare in open clusters
Deacon, N. R., & Kraus, A. L. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1877 · Cited by 59
“Star formation is broadly categorised into clustered enviroments that are the likely progenitors of the open clusters we see in the solar neighbourhood and lower density distributed environments such as Sco-Cen or Taurus-Auriga.”
BackgroundInfluentialSelf-citationThe SPHERE view of the Taurus star-forming region
Garufi, A., Ginski, C., van Holstein, R. G., Benisty, M., Manara, C. F., Sebastian Perez, M., Pinilla, P., Ribas, Á., Weber, P., Williams, J. P., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347586 · Cited by 58
CHARACTERIZING THE STELLAR PHOTOSPHERES AND NEAR-INFRARED EXCESSES IN ACCRETING T TAURI SYSTEMS
McClure, M. K., Calvet, N., Espaillat, C. C., Hartmann, L., Hernández, J., Ingleby, L., Luhman, K. L., D'Alessio, P., & Sargent, B. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/769/1/73 · Cited by 58
“The CTTS are all single stars, within a detection limit of ∆mK=2 at separations greater than 20 mas, while the WTTS, LkCa 3 and V827 Tau, are subarcsecond binaries (Kraus et al. 2011).”
BackgroundMethodThermal Jeans Fragmentation within ∼1000 au in OMC-1S
Palau, A., Zapata, L. A., Román-Zúñiga, C. G., Sánchez-Monge, Á., Estalella, R., Busquet, G., Girart, J. M., Fuente, A., & Commerçon, B. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaad03 · Cited by 58
“However, this behavior seems to be different from the Taurus cloud (Kraus et al. 2011), and should not necessary apply to Orion.”
BackgroundBlack hole and neutron star mergers in galactic nuclei: the role of triples
Fragione, G., Leigh, N. W. C., & Perna, R. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1803 · Cited by 57
DYNAMICAL MASSES OF YOUNG STARS. I. DISCORDANT MODEL AGES OF UPPER SCORPIUS
Rizzuto, A. C., Ireland, M., Dupuy, T. J., & Kraus, A. L. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/817/2/164 · Cited by 57
“…science goals, such as circumstellar disk evolution (Carpenter et al. 2009; Chen et al. 2011; Rizzuto et al. 2012), exoplanet identification and evolution (Lafrenière et al. 2008, 2009; Ireland et al. 2011) and multiplicity studies (Kouwenhoven et al. 2007; Kraus et al. 2011; Rizzuto et al. 2013).”
BackgroundSelf-citationFormation of wide binary stars from adjacent cores
Tokovinin, A. A. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx707 · Cited by 57
“Kraus et al. (2011) also studied the separation distribution in Taurus, but only out to 5 kAU, avoiding the clustering regime.”
BackgroundRESOLVING THE GAP AND AU-SCALE ASYMMETRIES IN THE PRE-TRANSITIONAL DISK OF V1247 ORIONIS
Kraus, S., Ireland, M., Sitko, M. L., Monnier, J. D., Calvet, N., Espaillat, C. C., Grady, C. A., Harries, T. J., Hönig, S. F., Russell, R. W., et al. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/768/1/80 · Cited by 56
“The error estimation and detection limits in our code have been carefully tested and fine-tuned in various earlier studies (e.g. Kraus et al. 2011; Kraus & Ireland 2012).”
MethodSelf-citationLacour, S., Tuthill, P., Amico, P., Ireland, M., Ehrenreich, D., Huélamo, N., & Lagrange, A. ‐. (2011) · arXiv (Cornell University) · doi:10.48550/arxiv.1107.1426 · Cited by 67
“These results confirm previous detection limits obtained by the same aperture masking technique on the Keck telescope (Kraus et al. 2011; Hinkley et al. 2011) In terms of scientific impact, this observational domain is important because it corresponds to a few astronomical units at a hundred…”
ResultSelf-citationMergerburst transients of brown dwarfs with exoplanets
Bear, E., Kashi, A., & Soker, N. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.19171.x · Cited by 55
“BDs are known to exist also in binary systems, both as the less massive component and as the primary (e.g., Thies et al. 2010; Kraus et al. 2011).”
BackgroundCieza, L. A., Olofsson, J., Harvey, P. M., Evans, N. J., Najita, J., Henning, T. K., Merín, B., Liebhart, A., Güdel, M., Augereau, J. ‐., et al. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/762/2/100 · Cited by 55
“For example, disks in close binary systems disappear more rapidly (Cieza et al. 2009; Kraus et al. 2011), and different initial core properties and evolution during the embedded phase can affect the disk evolution (Dunham & Vorobyov 2012).”
BackgroundA PAN-STARRS + UKIDSS SEARCH FOR YOUNG, WIDE PLANETARY-MASS COMPANIONS IN UPPER SCORPIUS
Aller, K. M., Kraus, A. L., Liu, M. C., Burgett, W. S., Chambers, K. C., Hodapp, K. W., Kaiser, N., Magnier, E. A., & Price, P. A. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/773/1/63 · Cited by 55
“Therefore we would expect that their separation distribution would be similar to that for stars and brown dwarfs (Kraus et al. 2011) such that their distribution would be logarithmically flat (i.e. companion masses are equally likely in log(separation)).”
BackgroundSelf-citationSUB-STELLAR COMPANIONS AND STELLAR MULTIPLICITY IN THE TAURUS STAR-FORMING REGION
Daemgen, S., Bonavita, M., Jayawardhana, R., Lafreniére, D., & Janson, M. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/799/2/155 · Cited by 54
“Previous studies of Taurus (see, e.g., Kraus et al. 2011, and references therein) have found a large number of multiple systems in the region, with a much higher frequency of wide binary companions than in denser clusters and the field (Kraus & Hillenbrand 2007, 2009b).”
BackgroundResultInfluentialSpin-orbit angle distribution and the origin of (mis)aligned hot Jupiters
Crida, A., & Batygin, K. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201323292 · Cited by 53
“…isotropic, the binary semi-major axis is drawn from a log-flat distribution spanning 102.5 − amax AU (where amax can vary, see caption of Figure 6 ; Kraus et al. 2011), while the eccentricity and the primary-to-perturber mass ratio are taken to be uniform in the intervals [0,1] and [0.1,10],…”
BackgroundInfluentialTobin, J. J., Offner, S. S. R., Kratter, K. M., Megeath, S. T., Sheehan, P., Looney, L. W., Díaz-Rodríguez, A. K., Osorio, M., Anglada, G., Sadavoy, S., et al. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac36d2 · Cited by 54
Protoplanetary Disk Masses from Stars to Brown DwarfsPreprint
Mohanty, S., Greaves, J. S., Mortlock, D. J., Pascucci, I., Scholz, A., Thompson, M. A., Apai, D., & Looper, D. L. (2016) · Cited by 54
Hinkley, S., Carter, A. L., Ray, S., Skemer, A. J. I., Biller, B. A., Choquet, É., Millar‐Blanchaer, M. A., Sallum, S., Miles, B., Whiteford, N., et al. (2022) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/ac77bd · Cited by 53
Self-citationMAPPING THE SHORES OF THE BROWN DWARF DESERT. IV. OPHIUCHUS
Cheetham, A. C., Kraus, A. L., Ireland, M., Cieza, L. A., Rizzuto, A. C., & Tuthill, P. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/813/2/83 · Cited by 53
“Our results reflect that of Ratzka et al. (2005), who found significant differences in stellar multiplicity between the Ophiuchus and Taurus-Auriga star forming regions.”
InfluentialSelf-citationBryan, M. L., Bowler, B. P., Knutson, H. A., Kraus, A. L., Hinkley, S., Mawet, D. P., Nielsen, E. L., & Blunt, S. C. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/827/2/100 · Cited by 52
“Efforts using non-redundant aperture masking techniques have probed higher masses (>15 MJup) down to smaller separations (> ∼ 5 AU), and have likewise found a dearth of inner companions (Cheetham et al 2015; Kraus et al 2011).”
BackgroundSelf-citationKing, R. R., Goodwin, S. P., Parker, R. J., & Patience, J. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.22108.x · Cited by 52
“Another interesting feature is that they all appear to be roughly flat in log-space (see Kraus et al. 2008, 2011), although there is a tendency to have more low-separation (19–50 au) binaries than expected from a completely log-flat distribution.”
BackgroundInfluentialThe Origin of the Stellar Mass Distribution and Multiplicity
Lee, Y.-N., Offner, S. S. R., Hennebelle, P., André, P., Zinnecker, H., Ballesteros‐Paredes, J., Inutsuka, S.-I., & Kruijssen, J. M. D. (2020) · Space Science Reviews · doi:10.1007/s11214-020-00699-2 · Cited by 51
Orbital Parameter Determination for Wide Stellar Binary Systems in the Age of Gaia
Pearce, L. A., Kraus, A. L., Dupuy, T. J., Mann, A. W., Newton, E. R., Tofflemire, B. M., & Vanderburg, A. M. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab8389 · Cited by 51
“High-resolution imaging has ruled out additional stellar companions to either source down to ρ∼5 au (Kraus et al. 2011).”
BackgroundInfluentialSelf-citationACCRETION AND MAGNETIC RECONNECTION IN THE CLASSICAL T TAURI BINARY DQ TAU
Tofflemire, B. M., Mathieu, R. D., Ardila, D. R., Akeson, R., Ciardi, D. R., Johns‐Krull, C. M., Herczeg, G. J., & Quijano-Vodniza, A. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/835/1/8 · Cited by 49
“Kraus et al. (2011), for instance, find that up to 75% of Class II/III members of the Taurus-Auriga star-forming region are in multi-star systems.”
BackgroundMultiplicity and clustering in Taurus star-forming region
Joncour, I., Duchêne, G., & Moraux, E. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201629398 · Cited by 49
SPECTRAL ENERGY DISTRIBUTIONS OF ACCRETING PROTOPLANETS
Eisner, J. A. (2015) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/803/1/l4 · Cited by 48
“While many transition disks have no detected planets despite observations with the required contrast (e.g., Kraus et al. 2011; Evans et al. 2012), observations probed a limited semimajor axis range.”
BackgroundSearch for associations containing young stars (SACY)
Elliott, P., Huélamo, N., Bouy, H., Bayo, A., Melo, C., Torres, C. A. O., Sterzik, M., Quast, G. R., Chauvin, G., & Barrado, D. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201525794 · Cited by 48
“Left: Red, green and gold shaded areas represent the 68% confidence intervals for the kernel density estimation (KDE) of multiple systems for SACY, Taurus (K11) and the field (R10), respectively.”
BackgroundResultInfluentialIs stellar multiplicity universal? Tight stellar binaries in the Orion Nebula Cluster
Duchêne, G., Lacour, S., Moraux, E., Goodwin, S. P., & Bouvier, J. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1180 · Cited by 47
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
Transition disks: the observational revolution from SEDs to imaging
van der Marel, N. (2023) · The European Physical Journal Plus · doi:10.1140/epjp/s13360-022-03628-0 · Cited by 47
“The discovery of the 8 au stellar companion inside the 14 au cavity of CoKu Tau/4 [38] initially led to the suggestion that all transition disks might be circumbinary disks, and a binary companion was also discovered for HD142527 [39, 40], but firm limits on companions in several transition disk cavities made this unl…”
BackgroundGeller, A. M., de Grijs, R., Li, C., & Hurley, J. R. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/779/1/30 · Cited by 46
“…of star-forming regions, young and old star clusters, and the Galactic field indicate that most stars reside in binary or higher-order multiple systems (e.g. Kouwenhoven et al. 2005, 2007; Raghavan et al. 2010; Geller et al. 2010; Kraus et al. 2011; Geller & Mathieu 2012; King et al. 2012).”
The central 1000 au of a pre-stellar core revealed with ALMA. I. 1.3 mm continuum observations
Caselli, P., Pineda, J. E., Zhao, B., Walmsley, M. C., Keto, E., Tafalla, M., Chacón-Tanarro, A., Bourke, T. L., Friesen, R., Galli, D., et al. (2019) · MPG.PuRe (Max Planck Society) · Cited by 46
DISCOVERY OF A VERY LOW MASS TRIPLE WITH LATE-M AND T DWARF COMPONENTS: LP 704-48/SDSS J0006−0852AB
Burgasser, A., Luk, C., Dhital, S., Gagliuffi, D. B. B., Nicholls, C., Prato, L., West, A., & Lépine, S. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/757/2/110 · Cited by 34
“…most stars form in multiple systems, with the frequency, mass ratio distribution and period distribution of multiples varying as a function of mass and possibly formation environment (e.g., Delgado-Donate et al. 2004; Ahmic et al. 2007; Burgasser et al. 2007b; Bate 2009, 2012; Kraus et al. 2011).”
BackgroundYoudin, A. N., & Kenyon, S. J. (2013) · Springer eBooks · doi:10.1007/978-94-007-5606-9_1 · Cited by 54
“Despite the current lack of large samples of planets in this domain, direct imaging surveys are starting to discover 1–30 MJ objects with a ∼ 10–100 AU (Kalas et al. 2008; Marois et al. 2008; Lagrange et al. 2010; Currie et al. 2010; Kraus et al. 2011).”
BackgroundZurlo, A., Cieza, L. A., Sebastian Perez, M., Christiaens, V., Williams, J. P., Guidi, G., Cánovas, H., Casassus, S., Hales, A. S., Principe, D. A., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1886 · Cited by 46
“In Taurus, for example, the frequency of multiple systems is ∼70% (Kraus et al. 2011).”
BackgroundKing, R. R., Goodwin, S. P., Parker, R. J., & Patience, J. (2012) · White Rose Research Online (University of Leeds, The University of Sheffield, University of York) · Cited by 45
CIRCUMSTELLAR DISKS AROUND BINARY STARS IN TAURUSPreprint
Akeson, R., & Jensen, E. L. N. (2016) · Cited by 45
Resolving structure of the disc around HD100546 at 7 mm with ATCA
Wright, C. M., Maddison, S., Wilner, D. J., Burton, M., Lommen, D., van Dishoeck, E. F., Pinilla, P., Bourke, T. L., Ménard, F., & Walsh, C. M. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1619 · Cited by 43
“Kraus et al. (2011) quote a mass ratio of 0.009 within most of the cavity, which translates into a secondary mass of 14 MJ using their preferred primary mass of 1.46 M , or up to 19 MJ assuming a stellar mass of 2 M also found in the literature.”
BackgroundInfluentialORBITAL MONITORING OF THE ASTRALUX LARGE M-DWARF MULTIPLICITY SAMPLE
Janson, M., Bergfors, C., Brandner, W., Bonnefoy, M., Schlieder, J. E., Köhler, R., Hormuth, F., Henning, T. K., & Hippler, S. (2014) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/214/2/17 · Cited by 44
“This has led to a significant amount of multiplicity studies in recent years, spanning a wide range of stellar masses (e.g., Burgasser et al. 2007; Raghavan et al. 2010; Kraus et al. 2011; Janson et al. 2013; De Rosa et al. 2014).”
Background(董若冰), R. D., & Dawson, R. I. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/825/1/77 · Cited by 42
“Recent near-IR interferometry (Pott et al. 2010), adaptive optics imaging (Cieza et al. 2012), and aperture masking observations (Kraus et al. 2011) have shown that the observed inner holes and gaps in transitional disks are rarely due to close stellar companions or brown dwarfs (Alexander et al.…”
BackgroundEmbedded binaries and their dense cores
Sadavoy, S., & Stahler, S. W. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1061 · Cited by 43
“Populations of multiple star systems at the main sequence and pre-main sequence stages have been well studied in various clouds (e.g., Duquennoy & Mayor 1991; Raghavan et al. 2010; Kraus et al. 2011), revealing variations in binary frequency with stellar mass (Lada 2006; Duchêne & Kraus 2013).”
BackgroundDANCING IN THE DARK: NEW BROWN DWARF BINARIES FROM KERNEL PHASE INTERFEROMETRY
Pope, B. J. S., Martinache, F., & Tuthill, P. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/767/2/110 · Cited by 42
“This is the low-mass end of the ‘brown dwarf desert’ first identified by Marcy & Butler (2000), which has since become the subject of intense study (Grether & Lineweaver 2006; Allen et al. 2007; Kraus et al. 2008; Deleuil et al. 2008; Kraus et al. 2011; Dieterich et al. 2012; Evans et al. 2012).”
BackgroundSelf-citationDupuy, 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-citationGap, shadows, spirals, and streamers: SPHERE observations of binary-disk interactions in GG Tauri A
Keppler, M., Penzlin, A. B. T., Benisty, M., van Boekel, R., Henning, T. K., van Holstein, R. G., Kley, W., Garufi, A., Ginski, C., Brandner, W., et al. (2020) · Springer Link (Chiba Institute of Technology) · doi:10.3929/ethz-b-000428484 · Cited by 42
The curiously circular orbit of Kepler-16b
Dunhill, A., & Alexander, R. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt1456 · Cited by 17
“At larger separations (a & 10 au), where young binaries are more readily observed, most circumbinary discs appear to be rather low mass: the majority of the circumbinary discs identified by Kraus et al. (2011, 2012) have masses Md 6 10−3 M (Andrews & Williams 2005).”
BackgroundThe Formation Conditions of the Wide Binary Class 0 Protostars within BHR 71
Tobin, J. J., Bourke, T. L., Mader, S., Kristensen, L. E., Arce, H. G., Gueth, F., Gusdorf, A., Codella, C., Leurini, S., & Chen, X. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaef87 · Cited by 41
“…of multiple star formation in the main-sequence, pre-main sequence phase, and even the protostellar phase are becoming much better characterized (Kraus et al. 2011; Raghavan et al. 2010; Ward-Duong et al. 2015; Chen et al. 2013; Tobin et al. 2016), the physical processes that lead to multiple…”
BackgroundTofflemire, B. M., Mathieu, R. D., & Johns‐Krull, C. M. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab4f7d · Cited by 41
“Corresponding author: Benjamin M. Tofflemire tofflemire@utexas.edu Binary systems, however, are a common outcome of star formation (Raghavan et al. 2010; Kraus et al. 2011) that can fundamentally alter the canonical star-disk interaction.”
BackgroundThe IGRINS YSO Survey. I. Stellar Parameters of Pre-main-sequence Stars in Taurus-Auriga
López–Valdivia, R., Sokal, K. R., Mace, G. N., Kidder, B. T., Hussaini, M., Nofi, L., Prato, L. A., Johns‐Krull, C. M., Oh, H., Lee, J., et al. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac1a7b · Cited by 41
Self-citationKounkel, M., Megeath, S. T., Poteet, C. A., Fischer, W. J., & Hartmann, L. W. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/821/1/52 · Cited by 41
Magnetic field, activity, and companions of V410 Tau
Yu, L., Donati, J. ‐., Grankin, K. N., Cameron, A. C., Moutou, C., Hussain, G. A. J., Baruteau, C., & Jouve, L. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2481 · Cited by 44
“…could support the hypothesis that V410 Tau B, although having a slightly lower mass ratio (q = 0.2 ± 0.1, MNRAS 000, 1–28 (2018) Mag. field, activity & companions of V410 Tau 17 Kraus et al. 2011), played a role in the early disc dissipation, which in turn prevented the formation of a hot Jupiter.”
BackgroundInfluentialSimulations of star formation in Ophiuchus – II. Multiplicity
Lomax, O., Whitworth, A. P., Hubber, D. A., Stamatellos, D., & Walch, S. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu2530 · Cited by 38
“Observations of young embedded populations also reveal many high-order multiples including sextuples (e.g. Kraus et al. 2011), but the statistics are too poor to merit a parametric fit.”
BackgroundResultInfluentialFernandez, M. A., Covey, K. R., Lee, N. D., Chojnowski, S. D., Nidever, D. L., Ballantyne, R., Cottaar, M., Rio, N. D., Foster, J. B., Majewski, S. R., et al. (2017) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/aa77e0 · Cited by 38
“…Kraus & Hillenbrand 2009; Vogt et al. 2012; Ward-Duong et al. 2015), as well as imaging enhanced with speckle (e.g., Ghez et al. 1993, 1997; Ratzka et al. 2005), aperture masking (Kraus et al. 2008, 2011; Cheetham et al. 2015), and multi-aperture interferometric (Guenther et al. 2007) techniques.”
BackgroundK2-231 b: A Sub-Neptune Exoplanet Transiting a Solar Twin in Ruprecht 147
Curtis, J. L., Vanderburg, A. M., Torres, G., Kraus, A. L., Huber, D., Mann, A. W., Rizzuto, A. C., Isaacson, H., Howard, A. W., Henze, C. E., et al. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aab49c · Cited by 35
“For the target and reference star, we obtained four (three) interferograms for a total of 80 (60)s on K2-231 (EPIC 219511354), which we analyzed following Kraus et al. (2008, 2011, 2016).”
MethodSelf-citationVLTI/MIDI atlas of disks around low- and intermediate-mass young stellar objects
Varga, J., Ábrahám, P., Chen, L., Ratzka, T., Gabányi, K. É., Kóspál, Á., Matter, A., van Boekel, R., Henning, T. K., Jaffe, W., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201832599 · Cited by 38
Unveiling the star formation history of the Upper Scorpius association through its kinematics
Squicciarini, V., Gratton, R., Bonavita, M., & Mesa, D. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2079 · Cited by 38
GG Tau: the ringworld and beyond
Dutrey, A., Folco, E. D., Beck, T. L., & Guilloteau, S. (2016) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-015-0091-5 · Cited by 37
The non-monotonic, strong metallicity dependence of the wide-binary fraction
Hwang, H.-C., Ting, Y.-S., Schlaufman, K. C., Zakamska, N. L., & Wyse, R. F. Ġ. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3854 · Cited by 37
An Improved Hertzsprung–Russell Diagram for the Orion Trapezium Cluster
Fang, M., Kim, J. S., Pascucci, I., & Apai, D. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abcec8 · Cited by 37
Zurlo, A., Cieza, L. A., Ansdell, M., Christiaens, V., Sebastian Perez, M., Lovell, J. B., Mesa, D., Williams, J. P., González-Ruilova, C., Carraro, R., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3674 · Cited by 37
Mass 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
“The analysis for the SAM data was identical to that used in previous papers (e.g., Ireland & Kraus 2008; Kraus et al. 2008, 2011), combined with the new calibration technique described in Kraus & Ireland (2012).”
MethodSelf-citationThe Effect of Binarity on Circumstellar Disk Evolution
Barenfeld, S. A., Carpenter, J. M., Sargent, A. I., Rizzuto, A. C., Kraus, A. L., Meshkat, T., Akeson, R. L., Jensen, E. L. N., & Hinkley, S. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab1e50 · Cited by 36
Self-citationB- AND A-TYPE STARS IN THE TAURUS-AURIGA STAR-FORMING REGION
Mooley, K., Hillenbrand, L., Rebull, L., Padgett, D., & Knapp, G. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/771/2/110 · Cited by 36
“…dwarf candidate members (Rebull et al. 2010, 2011; Luhman et al. 2009, 2010; Takita et al. 2010) as well as new companions to already known objects (Kraus et al. 2011), (4) measurement of proper motions using optical and VLBI techniques (Torres et al. 2009; Luhman et al. 2009), (5) provision of…”
MethodSelf-citationGuszejnov, D., Hopkins, P. F., & Krumholz, M. R. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx725 · Cited by 36
“Both observations (Duchêne 1999; Kraus et al. 2008, 2011) and simulations have shown that stars are born in complex, multiple systems that are broken up by dynamical effects (e.g., ejection of stars) causing multiplicity to drop (Goodwin et al. 2007; Kaczmarek et al. 2011) and the period…”
BackgroundSubstellar multiplicity in the Hyades cluster
Duchêne, G., Bouvier, J., Moraux, E., Bouy, H., Konopacky, Q., & Ghez, A. M. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201321691 · Cited by 35
“This is reminiscent of findings among both field systems, where several empirical “maximum separation” laws have been proposed (Reid et al. 2001; Burgasser et al. 2003; Close et al. 2003), and star-forming regions (e.g., Kraus et al. 2011).”
ResultPulsed Accretion in the T Tauri Binary TWA 3A
Tofflemire, B. M., Mathieu, R. D., Herczeg, G. J., Akeson, R., & Ciardi, D. R. (2017) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aa75cb · Cited by 35
“Table 1 presents the relevant binary and disk characteristics for TWA 3A. Binary and higher-order multiple systems are observed as a frequent outcome of star formation (Raghavan et al. 2010; Kraus et al. 2011).”
BackgroundDisk Material Inflates Gaia RUWE Values in Single Stars
Fitton, S., Tofflemire, B. M., & Kraus, A. L. (2022) · Research Notes of the AAS · doi:10.3847/2515-5172/ac4bb7 · Cited by 35
Self-citationSPARSE APERTURE MASKING OBSERVATIONS OF THE FL Cha PRE-TRANSITIONAL DISK
Cieza, L. A., Lacour, S., Schreiber, M. R., Casassus, S., Jordán, A., Mathews, G. S., Cánovas, H., Ménard, F., Kraus, A. L., Pérez, S., et al. (2012) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/762/1/l12 · Cited by 34
“Since pre-transitional disks tend to lack stellar companions (Pott et al. 2010; Kraus et al. 2011), their gaps are best explained by the dynamical interaction of unseen substellar or planetary-mass objects embedded in the disk (Dobson-Robinson & Salyk, 2012).”
BackgroundSelf-citationElliott, P., & Bayo, A. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw926 · Cited by 33
“This is supported by the conservation of the MF and CSF quantities in larger separation ranges for Class 0 sources (15-10,000 au, Tobin et al. 2016), Class I/II/III sources (3-5000 au, Kraus et al. 2011) and Class III sources (≈0.01-100,000 au, this work).”
BackgroundInfluentialBinary star formation and the outflows from their discs
Kuruwita, R. L., Federrath, C., & Ireland, M. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1299 · Cited by 33
“…stars with effective temperature between 4800 K and 6550 K, the multiplicity of field stars is approximately 50–60 per cent (Duquennoy & Mayor 1991; Kraus et al. 2011), while lower mass stars and dwarfs have a multiplicity of 30 per cent down to 10 per cent (Lada 2006; Basri & Reiners 2006; Ahmic…”
BackgroundSelf-citationBowler, B., & Hillenbrand, L. (2015) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/811/2/l30 · Cited by 24
“2M0441+2301Aab has undergone significant changes in separation of 1.4 ± 0.2 mas yr−1 and in position angle (P.A.) of –1.3 ± 0.02◦ yr−1 since 2008 (Kraus et al. 2011; Todorov et al. 2010; Todorov et al. 2014).”
BackgroundInfluentialSelf-citationVLTI/MIDI atlas of disks around low- and intermediate-mass young stellar objects
Varga, J., Ábrahám, P., Chen, L., Ratzka, T., Gabányi, K. É., Kóspál, Á., Matter, A., van Boekel, R., Henning, T. K., Jaffe, W., et al. (2018) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · doi:10.1051/0004-6361/201832599/pdf · Cited by 32
Effects of the environment on the multiplicity properties of stars in the STARFORGE simulations
Guszejnov, D., Raju, A. N., Offner, S. S. R., Grudić, M. Y., Faucher‐Giguère, C., Hopkins, P. F., & Rosen, A. L. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3268 · Cited by 32
Pearce, L., Kraus, A. L., Dupuy, T. J., Ireland, M., Rizzuto, A. C., Bowler, B. P., Birchall, E. K., & Wallace, A. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/aafacb · Cited by 33
Self-citationSPYGLASS. IV. New Stellar Survey of Recent Star Formation within 1 kpc
Kerr, R. M. P., Kraus, A. L., & Rizzuto, A. C. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/ace5b3 · Cited by 31
Self-citationCieza, L., Mathews, G., Williams, J. P., Ménard, F., Kraus, A., Schreiber, M., Romero, G. A., Orellana, M., & Ireland, M. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/752/1/75 · Cited by 24
“The data analysis was identical to that used in previous papers (e.g., Ireland et al. 2008; Kraus et al. 2008, 2011), combined with the new calibration technique described in Kraus & Ireland (2012).”
MethodSelf-citationOn the sensitivity of closure phases to faint companions in optical long baseline interferometry
Bouquin, J.-B. L., & Absil, O. (2012) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201117891 · Cited by 31
“This result can be compared with the survey for stellar and sub-stellar companions on the ten-metre Keck and five-metre Palomar telescopes using aperture masking techniques in the K band (Kraus et al. 2008, 2011).”
ResultConsistent dust and gas models for protoplanetary disks
Dionatos, O., Woitke, P., Güdel, M., Degroote, P., Liebhart, A., Anthonioz, F., Antonellini, S., Baldovin-Saavedra, C., Carmona, A., Dominik, C., et al. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201832860 · 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
Self-citationA pilot survey of the binarity of Massive Young Stellar Objects withK-band adaptive optics
Pomohaci, R., Oudmaijer, R. D., & Goodwin, S. P. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz014 · Cited by 30
“Both the MF and CF of MYSOs determined from NaCo are higher than those of Kraus et al. (2011) within the same range, continuing the field star trend of multiplicity increasing with mass (for the same evolutionary stage).”
BackgroundInfluentialGW Orionis: Inner disk readjustments in a triple system
Fang, M., Sicilia‐Aguilar, A., Roccatagliata, V., Fedele, D., Henning, T. K., Eiroa, C., & Müller, A. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201424146 · Cited by 29
“Kraus et al. (2011) 30).”
BackgroundThe Taurus Boundary of Stellar/Substellar (TBOSS) Survey
Bulger, J., Patience, J., Ward-Duong, K., Pinte, C., Bouy, H., Ménard, F., & Monin, J.-L. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201323088 · Cited by 29
“Based on high resolution imaging, both the primary and secondary of the J04414565/J04414489 system posses close companions, while neither the primary nor secondary of the J04554757/J04554801 system has a close companion (Kraus et al. 2011; Todorov et al. 2014).”
BackgroundMethodEclipsing Binaries in the Open Cluster Ruprecht 147. I. EPIC 219394517
Torres, G., Curtis, J. L., Vanderburg, A. M., Kraus, A. L., & Rizzuto, A. C. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aadca8 · Cited by 28
“We obtained and analyzed eight interferograms exposed for 20 s each, following observing and analysis procedures described by Kraus et al. (2008, 2011, 2016) and Rizzuto et al. (2016).”
MethodSelf-citationPRECISE HIGH-CADENCE TIME SERIES OBSERVATIONS OF FIVE VARIABLE YOUNG STARS IN AURIGA WITHMOST
Cody, A. M., Tayar, J., Hillenbrand, L. A., Matthews, J. M., & Kallinger, T. (2013) · The Astronomical Journal · doi:10.1088/0004-6256/145/3/79 · Cited by 27
“A direct imaging study determined ∆K=0.87 for this system (Kraus et al. 2011). lying white noise.”
BackgroundMethodInfluentialSelf-citationWisniewski, J. P., Ge, J., Crepp, J. R., Lee, N. D., Eastman, J. D., Esposito, M., Fleming, S. W., Gaudi, B. S., Ghezzi, L., Hernández, J. I. G., et al. (2012) · The Astronomical Journal · doi:10.1088/0004-6256/143/5/107 · Cited by 23
“…et al. 2009; Biller et al. 2010; Janson et al. 2011; Wahhaj et al. 2011), while the mass distribution of very low mass stellar companions has been explored by high contrast imaging (Kraus et al. 2011), spectroscopic (Duquennoy & Mayor 1991), and interferometric (Raghavan et al. 2010) studies.”
BackgroundInfluentialDemographics of Triple Systems in Dense Star Clusters
Fragione, G., Martinez, M. A. S., Kremer, K., Chatterjee, S., Rodriguez, C. L., Ye, C. S., Weatherford, N. C., Naoz, S., & Rasio, F. A. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/aba89b · Cited by 26
“Kraus et al. (2011) performed a highresolution imaging study to characterize the multiple-star populations in Taurus-Auriga.”
BackgroundLi, Y., Kouwenhoven, M. B. N., Stamatellos, D., & Goodwin, S. P. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/805/2/116 · Cited by 25
“…found to be of higher multiplicity, both in embedded and young star forming regions (e.g., Kraus & Hillenbrand 2007; Connelley et al. 2008a, 2008b; Kraus et al. 2011) and in the older stellar populations (e.g., Correia et al. 2006; Tokovinin et al. 2006; Eggleton & Tokovinin 2008; Law et al.…”
BackgroundSallum, S., Eisner, J. A., Close, L. M., Hinz, P. M., Skemer, A. J. I., Bailey, V. P., Briguglio, R. A., Follette, K. B., Males, J. R., Morzinski, K. M., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/801/2/85 · Cited by 24
“However, high resolution imaging has ruled out companions with masses higher than ∼20–30 MJup for approximately half of the known transition disks (Kraus et al. 2011; Evans et al. 2012).”
Geller, A. M., de Grijs, R., Li, C., & Hurley, J. R. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/805/1/11 · Cited by 24
“…multiple, stars are ubiquitous, and comprise a relatively large fraction of the stars in star forming regions (Ghez et al. 1993; Köhler et al. 2000; Kraus et al. 2011; Bate 2012; Sana et al. 2013), open clusters (Mermilliod et al. 1992; Patience et al. 1998, 2002; Geller et al. 2008, 2010; Hole…”
BackgroundHernández-Gómez, A., Loinard, L., Chandler, C. J., Rodríguez, L. F., Zapata, L. A., Wilner, D. J., Ho, P. T. P., Caux, E., Quénard, D., Bottinelli, S., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab0c97 · Cited by 23
Super resolution from diffraction limited images with kernel-phases
Martinache, F. (2012) · Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE · doi:10.1117/12.925883 · Cited by 22
Self-citationMassive Star Cluster Formation with Binaries. I. Evolution of Binary Populations
Cournoyer-Cloutier, C., Sills, A., Harris, W. E., Polak, B., Rieder, S., Andersson, E. P., Appel, S. M., Low, M. M., McMillan, S. L. W., & Zwart, S. P. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad90b3 · Cited by 22
Metadata
- Authors
- Kraus, A. L., Ireland, M. J., Martinache, F., & Hillenbrand, L. A.
- Affiliations
- University of Hawaiʻi at Mānoa (US)
- The University of Sydney (AU)
- National Astronomical Observatory of Japan (JP)
- California Institute of Technology (US)
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2011-03-17
- Volume
- 731
- Issue
- 1
- Pages
- 8
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W1996452021
- Semantic Scholar
- d9092295d91fdf71df1f34481bdbff65a7fb02f1
- Cited by
- 325
- References
- 133
- Citations by year
- 2026: 4 · 2025: 7 · 2024: 16 · 2023: 12 · 2022: 17 · 2021: 16 · 2020: 22 · 2019: 37 · 2018: 19 · 2017: 24 · 2016: 28 · 2015: 28 · 2014: 21 · 2013: 33 · 2012: 25
- FWCI
- 16.14
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- CaltechAUTHORS (California Institute of Technology) (submittedVersion)
- ANU Open Research (Australian National University) (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Science Foundation (NAS 5-26555)
- National Aeronautics and Space Administration (NAS 526555, 526555)
- California Institute of Technology
- Space Telescope Science Institute (NAS5- 26555, 5-26555, 26555)
- U.S. Naval Observatory (NAS 5-26555)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Keywords
- brown dwarf desert, multiple star formation, Taurus-Auriga star-forming region, binary companion, binary separation distribution, disk fragmentation, substellar companions
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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