NEW<i>UBVRI</i>PHOTOMETRY OF 234 M33 STAR CLUSTERS

Ma, Jun

doi:10.1088/0004-6256/145/4/88

Cited by 14 publications

(21 citation statements)

References 47 publications

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“…Using archival images of the Local Group Galaxies Survey (LGGS, Massey et al 2006) obtained using the 4 m Kitt Peak National Observatory telescope, Ma (2012) built a catalog of 392 clusters, and Ma (2013) added 234 others, all in the standard UBVRI photometric system. Fan & de Grijs (2014) also reanalyzed the LGGS photometry to publish a catalog of 708 clusters.…”

Section: The Cluster Datamentioning

confidence: 99%

“…Fan & de Grijs (2014) also reanalyzed the LGGS photometry to publish a catalog of 708 clusters. In this paper, we adopt for the UBVRI photometric system the Ma (2012Ma ( , 2013 photometry when available, and the Fan & de Grijs (2014) photometry for the other clusters, correcting the Fan & de Grijs (2014) photometric zero-points to the Ma (2012Ma ( , 2013 ones in order to have an homogeneous catalog. The zeropoint correction coefficients for Fan & de Grijs (2014) minus Ma (2012Ma ( , 2013 and ∆(V − I) = 0.086 mag, computed for respectively 289,208,208,250, and 178 clusters with available photometry in common between Fan & de Grijs (2014) and Ma (2012Ma ( , 2013 catalogs.…”

Section: The Cluster Datamentioning

confidence: 99%

“…To this end, we use three catalogs of clusters recently published in the literature: the San Roman et al (2010) catalog in the u * g r i z photometric system, and the Ma (2012Ma ( , 2013 and Fan & de Grijs (2014) catalogs in the standard UBVRI photometric system. We also use nearinfrared photometry that we derive from deep 2MASS images.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Deriving physical parameters of unresolved star clusters

Meulenaer

Narbutis

Mineikis

et al. 2015

A&A

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Context. When trying to derive the star cluster physical parameters of the M 33 galaxy using broad-band unresolved ground-based photometry, previous studies mainly made use of simple stellar population models, shown in the recent years to be oversimplified. Aims. In this study, we aim to derive the star cluster physical parameters (age, mass, and extinction; metallicity is assumed to be LMC-like for clusters with age below 1 Gyr and left free for older clusters) of this galaxy using models that take stochastic dispersion of cluster integrated colors into account. Methods. We use three recently published M 33 catalogs of cluster optical broad-band photometry in standard UBVRI and in CFHT/MegaCam u * g r i z photometric systems. We also use near-infrared JHK photometry that we derive from deep 2MASS images. We derive the cluster parameters using a method that takes into account the stochasticity problem, presented in previous papers of this series. Results. The derived differential age distribution of the M 33 cluster population is composed of a two-slope profile indicating that the number of clusters decreases when age gets older. The first slope is interpreted as the evolutionary fading phase of the cluster magnitudes, and the second slope as the cluster disruption. The threshold between these two phases occurs at ∼300 Myr, comparable to what is observed in the M 31 galaxy. We also model by use of artificial clusters the ability of the cluster physical parameter derivation method to correctly derive the two-slope profile for different photometric systems tested.

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Section: The Cluster Datamentioning

confidence: 99%

Section: The Cluster Datamentioning

confidence: 99%

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Deriving physical parameters of unresolved star clusters

Meulenaer

Narbutis

Mineikis

et al. 2015

A&A

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“…The star has been monitored at 23 epochs using the MARVELS instrument mounted on the SDSS 2.5m Telescope at APO between 2009 May and 2011 December (Ge et al 2008, Ma et al 2013. The MARVELS instrument is a fiber-fed dispersed fixeddelay interferometer instrument capable of observing 60 objects simultaneously and covers a wavelength range of 5000−5700Å with a resolution of R∼12,000.…”

Section: Marvels Rv Observationsmentioning

confidence: 99%

“…It was coupled to a wide field Sloan Digital Sky Survey telescope (SDSS, Gunn et al 2006) and used for the pilot Multi-Object APO Radial Velocity Exoplanet Large-Area Survey (MARVELS; Ge et al 2008Ge et al , 2009Ge & Eisenstein 2009-2007(Fleming et al 2010Eisenstein et al 2011). This is the sixth paper in this series examining the low-mass companions around solar type stars from the SDSS-III MARVELS survey (Wisniewski et al 2012;Fleming et al 2012;Ma et al 2013;Jiang et al 2013;De Lee et al 2013). In this paper, we present our discovery of two substellar companions, a giant planet (MARVELS-7b) and a brown dwarf (MARVELS-7c), around the primary star in a binary system, HD 87646, from the MARVELS pilot planet survey program.…”

Section: Introductionmentioning

confidence: 99%

Very Low-Mass Stellar and Substellar Companions to Solar-Like Stars From Marvels. Vi. A Giant Planet and a Brown Dwarf Candidate in a Close Binary System Hd 87646

Wolszczan

et al. 2016

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We report the detections of a giant planet (MARVELS-7b) and a brown dwarf candidate (MARVELS-7c) around the primary star in the close binary system, HD 87646. It is the first close binary system with more than one substellar circum-primary companion discovered to the best of our knowledge. The detection of this giant planet was accomplished using the first multi-object Doppler instrument (KeckET) at the Sloan Digital Sky Survey (SDSS) telescope. Subsequent radial velocity observations using ET at Kitt Peak National Observatory, HRS at HET, the "Classic" spectrograph at the Automatic Spectroscopic Telescope at Fairborn Observatory, and MARVELS from SDSS-III confirmed this giant planet discovery and revealed the existence of a long-period brown dwarf in this binary. HD 87646 is a close binary with a separation of ∼ 22 AU between the two stars, estimated using the Hipparcos catalogue and our newly acquired AO image from PALAO on the 200-inch Hale Telescope at Palomar. The primary star in the binary, HD 87646A, has T eff = 5770± 80K, log g =4.1±0.1 and [Fe/H] = −0.17 ± 0.08. The derived minimum masses of the two substellar companions of HD 87646A are 12.4±0.7 M Jup and 57.0±3.7 M Jup . The periods are 13.481±0.001 days and 674±4 days and the measured eccentricities are 0.05±0.02 and 0.50±0.02 respectively. Our dynamical simulations show the system is stable if the binary orbit has a large semi-major axis and a low eccentricity, which can be verified with future astrometry observations.

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Globular Clusters in the Local Group

Grebel

2014

Proc. IAU

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Only twelve of the > 76 Local Group galaxies contain globular clusters, showing a broad range of specific frequencies. Here we summarize the properties of these globular cluster systems. Many host galaxies contain very old globulars, but in some globular cluster formation may have been delayed. An age range of several Gyr is common. Except for the inner regions of the spirals, old globular clusters tend to be metal-poor. Increasingly, light element variations and hints of multiple stellar populations are being found also in extragalactic globulars. There is ample evidence for globular cluster accretion from dwarfs onto massive galaxies, but its magnitude has yet to be quantified. Caution is needed to avoid overinterpreting indirect evidence.

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NEWUBVRIPHOTOMETRY OF 234 M33 STAR CLUSTERS

Cited by 14 publications

References 47 publications

Deriving physical parameters of unresolved star clusters

Deriving physical parameters of unresolved star clusters

Very Low-Mass Stellar and Substellar Companions to Solar-Like Stars From Marvels. Vi. A Giant Planet and a Brown Dwarf Candidate in a Close Binary System Hd 87646

Globular Clusters in the Local Group

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