- ID:
- ivo://CDS.VizieR/J/ApJS/194/12
- Title:
- Trumpler 16 in the CCCP
- Short Name:
- J/ApJS/194/12
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Trumpler 16 is a well-known rich star cluster containing the eruptive supergiant {eta} Carinae and located in the Carina star-forming complex. In the context of the Chandra Carina Complex Project, we study Trumpler 16 using new and archival X-ray data. A revised X-ray source list of the Trumpler 16 region contains 1232 X-ray sources including 1187 likely Carina members. These are matched to 1047 near-infrared counterparts detected by the HAWK-I instrument at the Very Large Telescope allowing for better selection of cluster members. The cluster is irregular in shape. Although it is roughly circular, there is a high degree of sub-clustering, with no noticeable central concentration and an extension to the southeast. We estimate the total Trumpler 16 pre-main-sequence population to be >6500 Class II and Class III X-ray sources. An overall K-excess disk frequency of ~8.9% is derived using the X-ray-selected sample, although there is some variation among the sub-clusters, especially in the southeastern extension. X-ray emission is detected from 29 high-mass stars with spectral types between B2 and O3.
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Search Results
- ID:
- ivo://CDS.VizieR/J/AJ/159/105
- Title:
- Two new stellar associations in vicinity of the Sun
- Short Name:
- J/AJ/159/105
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this work we report the discovery of two new stellar associations in close vicinity of the Sun at roughly 180 and 150pc. These two associations, u-Tau assoc and e-Tau assoc, were detected based on their clustering in a multi-dimensional parameter space including {alpha}, {delta}, {mu}_{alpha}_, {mu}_{delta}_, and \bar{omega} of Gaia. The fitting of pre-main-sequence model isochrones in their color-magnitude diagrams suggests that the two associations are of about 50Myr old and the group members lower than ~0.8M_{sun}_ are at the stage of post-T Tauri.
- ID:
- ivo://CDS.VizieR/J/A+A/416/537
- Title:
- UBVI and HST photometry of young stellar clusters
- Short Name:
- J/A+A/416/537
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- These tables contain a combination of ground-based and HST archive data for stellar clusters in 18 nearby spiral galaxies. Structural parameters for each cluster are measured on HST images, while UBVI photometry is from ground-based data obtained with the Danish 1.54m telescope at ESO La Silla, the 2.56m Nordic Optical Telescope in La Palma, Canary Islands, and the 3m Shane Telescope at Lick Observatory, California. Photometry in the STMAG system based on the HST data is also given (table 7) for each cluster for the available bandpasses.
- ID:
- ivo://CDS.VizieR/J/A+A/407/919
- Title:
- UBVI and JHK photometry in Lindsay 1
- Short Name:
- J/A+A/407/919
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Results of UBVI stellar photometry of SMC star cluster Lindsay 1. The frames were obtained in October 1999 with the 1.3m Warsaw telescope, Las Campanas Observatory with the 2048x2048 CCD camera. Missing magnitudes and colors of the stars are replaced with value 100.00.
- ID:
- ivo://CDS.VizieR/J/A+A/435/65
- Title:
- UBVI photometry of NGC 6872 clusters population
- Short Name:
- J/A+A/435/65
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a photometric analysis of the rich star cluster population in the tidal tails of NGC 6872. We find star clusters with ages between 1-100Myr distributed in the tidal tails, while the tails themselves have an age of less than 150Myr. Most of the young massive (10^4^<=M/M_{sun}<=10^7^) clusters are found in the outer regions of the galactic disk or the tidal tails. The mass distribution of the cluster population can be well described by a power-law of the form N(m){prop.to}m^-alpha^, where alpha=1.85+/-0.11, in very good agreement with other young cluster populations found in a variety of different environments. We estimate the star formation rate for three separate regions of the galaxy, and find that the eastern tail is forming stars at ~2 times the rate of the western tail and ~5 times the rate of the main body of the galaxy. By comparing our observations with published N-body models of the fate of material in tidal tails in a galaxy cluster potential, we see that many of these young clusters will be lost into the intergalactic medium. We speculate that this mechanism may also be at work in larger galaxy clusters such as Fornax, and suggest that the so-called ultra-compact dwarf galaxies could be the most massive star clusters that have formed in the tidal tails of an ancient galactic merger.
- ID:
- ivo://CDS.VizieR/J/A+A/464/495
- Title:
- UBVI photometry of NGC 45 star clusters
- Short Name:
- J/A+A/464/495
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Star clusters are present in almost all types of galaxies. Here we investigate the star cluster population in the low-luminosity, unperturbed spiral galaxy NGC 45, which is located in the nearby Sculptor group. Both the old (globular) and young star-cluster populations are studied. Previous ground-based observations have suggested that NGC 45 has few if any "massive" young star clusters. We aim to study the population of lower-mass "open" star clusters and also identify old globular clusters that could not be distinguished from foreground stars in the ground-based data. Star clusters were identified using UBVI imaging from the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From broad band colors and comparison with simple stellar population (SSP) models assuming a fixed metallicity, we derived the age, mass, and extinction. We also measured the radius for each star cluster candidate.
- ID:
- ivo://CDS.VizieR/J/ApJ/452/210
- Title:
- UBV photometry in LH 47/48
- Short Name:
- J/ApJ/452/210
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We examine the stellar population of an OB association, LH 47/48, which is associated with a superbubble H II region, DEM 152 in the N44 nebular complex of the Large Magellanic Cloud. With CCD photometry and spectroscopy of the massive stars, we find no evidence that an unusual stellar population gave rise to the shell morphology of the gas. The slope of the initial mass function, {Gamma}=1.3+/-0.2, is consistent with that of other OB associations in the LMC, and there is no significant difference in the initial mass function internal or external to the supershell. The inferred stellar ionizing flux is consistent with the observed nebular H alpha flux. We do find evidence for triggered star formation: the H-R diagram suggests an age of >10Myr for the population interior to the bubble with more recent, <5Myr, star formation on the exterior. Using the detailed data on the stellar population, we compare a numerical form of the Weaver et al. (1977ApJ...218..377W) evolutionary model for wind-driven bubbles with the observed shell kinematics. We find a substantial discrepancy: the observed shell radius is too small and/or expansion velocity too large to be explained with this version of the model. We discuss possible explanations for the inconsistency.
- ID:
- ivo://CDS.VizieR/J/AJ/121/891
- Title:
- UBV photometry of LMC OB associations
- Short Name:
- J/AJ/121/891
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using ultraviolet photometry from the Ultraviolet Imaging Telescope (UIT) combined with photometry and spectroscopy from three ground-based optical data sets we have analyzed the stellar content of OB associations and field areas in and around the regions N79, N81, N83, and N94 in the Large Magellanic Cloud. In particular, we compare data for the OB association Lucke-Hodge 2 (LH 2) to determine how strongly the initial mass function (IMF) may depend on different photometric reductions and calibrations.
- ID:
- ivo://CDS.VizieR/J/A+AS/114/489
- Title:
- UBVRI CCD photometry of Cepheus OB3
- Short Name:
- J/A+AS/114/489
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Johnson CCD photometry was performed in the two subgroups of the association Cepheus OB3, for selected fields each containing at least one star with previous UBV photoelectric photometry. Photometry for about 1000 stars down to visual magnitude 21 is provided, although the completeness tests show that the sample is complete down to V=19mag. Individual errors were assigned to the magnitude and colours for each star. Colour-colour and colour-magnitude diagrams are shown. Astrometric positions of the stars are also given. Description of the reduction procedure is fully detailed.
- ID:
- ivo://CDS.VizieR/J/AJ/144/41
- Title:
- UBVRI photometry of M33 star clusters. I.
- Short Name:
- J/AJ/144/41
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present UBVRI photometry for 392 star clusters and candidates in the field of M33, which are selected from the most recent star cluster catalog. In this catalog, the authors listed star clusters' parameters such as cluster positions, magnitudes, colors in the UBVRIJHK_s_filters, and so on. However, a large fraction of objects in this catalog do not have previously published photometry. Photometry is performed using archival images from the Local Group Galaxies Survey, which covers 0.8deg^2^ along the major axis of M33. Detailed comparisons show that, in general, our photometry is consistent with previous measurements. Positions (right ascension and declination) for some clusters are corrected here. Combined with previous literature, ours constitute a large sample of M33 star clusters. Based on this cluster sample, we present some statistical results: none of the youngest M33 clusters (~10^7^yr) have masses approaching 10^5^M_{sun}_; roughly half the star clusters are consistent with the 10^4^-10^5^M_{sun}_ mass models; the continuous distribution of star clusters along the model line indicates that M33 star clusters have been formed continuously from the epoch of the first star cluster formation until recent times; and there are ~50 star clusters which are overlapped with the Galactic globular clusters on the color-color diagram, and these clusters are old globular cluster candidates in M33.
