The Stellar Populations of Praesepe and Coma Berenices

By A. Kraus, L. Hillenbrand. 2007

250 citations recorded by the source corpus.

We present the results of a stellar membership survey of the nearby open clusters Praesepe and Coma Berenices. We have combined archival survey data from the SDSS, 2MASS, USNOB1.0, and UCAC-2.0 surveys to compile proper motions and photometry for ∼5 million sources over 300 deg2. Of these sources, 1010 stars in Praesepe and 98 stars in Coma Ber are identified as candidate members with probability >80%; 442 and 61 are identified as high-probability candidates for the first time. We estimate that this survey is >90% complete across a wide range of spectral types (F0-M5 in Praesepe, F5-M6 in Coma Ber). We have also investigated the stellar mass dependence of each cluster's mass and radius in order to quantify the role of mass segregation and tidal stripping in shaping the present-day mass function and spatial distribution of stars. Praesepe shows clear evidence of mass segregation across the full stellar mass range; Coma Ber does not show any clear trend, but low number statistics would mask a trend of the same magnitude as in Praesepe. The mass function for Praesepe (τ ∼ 600 Myr; M ∼ 500 M⊙) follows a power law consistent with that of the field present-day mass function, suggesting that any mass-dependent tidal stripping could have removed only the lowest mass members (<0.15 M⊙). Coma Ber, which is younger but much less massive (τ ∼ 400 Myr; M ∼ 100 M⊙), follows a significantly shallower power law. This suggests that some tidal stripping has occurred, but the low-mass stellar population has not been strongly depleted down to the survey completeness limit (∼0.12 M⊙).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/790d7d963d13d2aa24fee761825e734d98d041f2

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In Astronomy and Astrophysics

1. Michael C. Liu
2. B. Bowler
3. A. Kraus
4. A. Mann
5. E. Gaidos
6. T. Dupuy
7. D. Huber
8. D. Charbonneau

In Instrumentation

1. Michael C. Liu
2. A. Mann
3. T. Dupuy
4. A. Kraus
5. E. Gaidos
6. K. Allers
7. Eric Mamajek
8. B. Bowler

Citations in the corpus

• SOAR TESS Survey. I. Sculpting of TESS Planetary Systems by Stellar Companions (2019, methodology): “We determine q by finding the mass of the primary star based on its likely spectral type estimated using the Teff reported in the TIC and the secondary star based on the magnitude difference with the primary (Kraus & Hillenbrand 2007).”
• A Universal Stellar Initial Mass Function? A critical look at variations in extreme environments (2010, background): “This wealth of low-mass members is also present in the Praesepe IMF constructed by Kraus & Hillenbrand (2007).”
• MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “A combination of its rich cluster membership (N & 1000; Kraus & Hillenbrand 2007), large proper motion, and proximity makes Prae- sepe a favorable target for stellar population studies.”
• BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, methodology): “…et al. 1999; (43) Pecaut & Mamajek 2013; (44) Elliott et al. 2014; (45) Webb et al. 1999; (46) Ducourant et al. 2014; (47) Pourbaix et al. 2004; (48) Kraus & Hillenbrand 2007; (49) Luhman & Steeghs 2004; (50) Shvonski et al. 2016; (51) Pecaut, priv. comm.; (52) Houk & Cowley 1975; (53)…”
• MAPPING THE SHORES OF THE BROWN DWARF DESERT. II. MULTIPLE STAR FORMATION IN TAURUS–AURIGA (2011, methodology): “We estimated the properties of our sample members using the method described in Kraus & Hillenbrand (2007a), specifically adapted for stars of the median age of Taurus (∼2 Myr; Kraus & Hillenbrand 2009b).”
• Planet Hunters IX. KIC 8462852-where's the flux? (2015, background): “This otherwise seemingly normal F-star undergoes erratic and completely unpredictable dips in flux ranging from 1 per cent to more than 20 per cent.”
• TWO WIDE PLANETARY-MASS COMPANIONS TO SOLAR-TYPE STARS IN UPPER SCORPIUS (2010, background): “Given that the total extinction along this line of sight is only AV ∼1.2 or E(J−K) ∼0.2 (Schlegel et al. 1998), the companion must be intrinsically cool (J − K &0.7 or spectral type &K5; Kraus & Hillenbrand 2007).”
• THE IMPACT OF STELLAR MULTIPLICITY ON PLANETARY SYSTEMS. I. THE RUINOUS INFLUENCE OF CLOSE BINARY COMPANIONS (2016, methodology): “0 (Monet et al. 2003), as described in Kraus & Hillenbrand (2007) and Kraus et al. (2014), to estimate both parameters.”
• 197 CANDIDATES AND 104 VALIDATED PLANETS IN K2's FIRST FIVE FIELDS (2016, methodology): “We estimate approximate spectral types (SpTs) using tabulated photometric relations (Kraus & Hillenbrand 2007; Pecaut & Mamajek 2013; Rodriguez et al. 2013) and convert SpTs into stellar radii (R*) based on interferometric studies (Boyajian et al. 2012).”
• THE MASS–RADIUS(–ROTATION?) RELATION FOR LOW-MASS STARS (2010, methodology): “For each system, we first used our composite spectral type (which represents the average of both components) to estimate a composite temperature from the temperature scale we reported in Kraus & Hillenbrand (2007).”
• THE ASTRALUX LARGE M-DWARF MULTIPLICITY SURVEY (2012, methodology): “…spectral type and relative photometry of each binary pair into individual spectral types and masses, we again follow the procedure in Bergfors et al. (2010), which was developed in Daemgen et al. (2007) and is based on the magnitude–spectral-type relationship in Kraus & Hillenbrand (2007).”
• A STELLAR CENSUS OF THE TUCANA–HOROLOGIUM MOVING GROUP (2014, methodology): “We describe the motivation and details in Kraus & Hillenbrand (2007).”
• A NEARBY M STAR WITH THREE TRANSITING SUPER-EARTHS DISCOVERED BY K2 (2015, methodology): “Using the riJHK photometric calibrations of Kraus & Hillenbrand (2007), we estimate a distance to K2-3 of 45± 3 pc.”
• Inverse dynamical population synthesis: Constraining the initial conditions of young stellar clusters by studying their binary populations (2012, background): “Kraus & Hillenbrand (2007) identify 1050 ± 30 Praesepe members earlier than spectral type M5, corresponding to 550± 40M⊙.”