On the Nature of the Hads Star V2455 Cyg

Peña, J. H.; Rentería, A.; Villarreal, Cuauhtémoc Calderón; Piña, D. S.

doi:10.22201/ia.01851101p.2019.55.02.07

Cited by 11 publications

(28 citation statements)

References 11 publications

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“…NGC 2343 is a third quadrant cluster situated near the Galactic midplane. Peña & Martínez (2014) showed the cluster to be young (12 Myr) and metal-poor, with [F e/H] ∼ −0.4 based on uvby − β photometry. It would be unusual for such a young cluster to be so metal-poor.…”

Section: Ngc 2343mentioning

confidence: 99%

The Swift UVOT Stars Survey. III. Photometry and Color–Magnitude Diagrams of 103 Galactic Open Clusters

Siegel

Porterfield

Hagen

et al. 2019

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As part of the Swift/UVOT Stars Survey, we present near-ultraviolet (3000-1700 A) point-source photometry for 103 Galactic open clusters. These data, taken over the span of the mission, provide a unique and unprecedented set of near-ultraviolet point-source photometry on simple stellar populations. After applying membership analysis fueled mostly by GAIA DR2 proper motions, we find that 49 of these 103 have clear precise CMDs amenable to investigation. We compare the CMDs to theoretical isochrones and find good agreement between the theoretical isochrones and the CMDs. The exceptions are the fainter parts of the main sequence and the red giant branch in the uvw2 − uvw1 CMDs, which is most likely due either to the difficulty of correcting for the red leak in the uvw2 filter or limitations in our understanding of UV opacities for cool stars. For the most part, our derived cluster parameters -age, distance and reddening -agree with the consensus literature but we find a few clusters that warrant substantial revision from literature values, notably NGC 2304, NGC 2343, NGC 2360, NGC 2396, NGC 2428, NGC 2509, NGC 2533, NGC 2571, NGC 2818, Collinder 220 and NGC 6939. A number of these are clusters in the third Galactic quadrant where previous studies have mistaken the disk sequence for the cluster. However, the GAIA DR2 proper motions clearly favor a different sequence. A number of clusters also show white dwarf and blue straggler sequences. We confirm the presence of extended main sequence turnoffs in NGC 2360 and NGC 2818 and show hints of it in a number of other clusters which may warrant future spectroscopic study. Most of the clusters in the study have low extinction and the rest are well fit by a "Milky-Way-like" extinction law. However, Collinder 220 hints at a possible "LMC-like" extinction law. We finally provide a comprehensive point-source catalog to the community as a tool for future investigation. arXiv:1905.04359v1 [astro-ph.SR] 10 May 2019Siegel et al.

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Section: Ngc 2343mentioning

confidence: 99%

The Swift UVOT Stars Survey. III. Photometry and Color–Magnitude Diagrams of 103 Galactic Open Clusters

Siegel

Porterfield

Hagen

et al. 2019

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“…The procedure to determine the physical parameters has been reported elsewhere (Peña et al, 2016). If the photometric system is well-defined and calibrated, it provides an efficient way to investigate physical conditions such as effective temperature and surface gravity via a direct comparison of the unreddened indexes with those obtained from the theoretical models.…”

Section: Data Acquisition and Reductionmentioning

confidence: 99%

“…The reduction was done considering the accuracy of the standard stars. As was stated in Peña et al (2016) reporting on BO Lyn, the observational pattern, as well as the reduction procedure, have been employed at the SPM Observatory since 1986 and hence, have been described many times. A detailed description of the methodology can be found in Peña et al (2007).…”

Section: Data Acquisition and Reductionmentioning

confidence: 99%

HD220735 and HD30110, new short period variable stars

Peña¹,

Soni²,

Rentería³

et al. 2019

IBVS

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“…The application of the calibrations for each spectral type (Balona & Shobbrook 1984;Shobbrook 1984) for O and early A type and Nissen (1988) for late A and F stars, respectively allowed us to determine their reddening, and hence their unreddened color indexes. The procedure has been extensively described in Peña & Martínez (2014). (Peña & Sareyan 2006).…”

Section: Methodsmentioning

confidence: 99%

“…The procedure followed has been extensively used and a description can be found in Peña et al (2008), Peña & Martinez (2014) or, more recently, in Peña et al (2017). What matters in the present paper are the coefficients of the transformation equations to the standard system and the numerical errors which provide the goodness and confidence of our numerical results.…”

Section: Data Acquisition and Reductionmentioning

confidence: 97%

STUDY OF THE OPEN CLUSTER NGC 1528 THROUGH uvby − β PHOTOELECTRIC PHOTOMETRY

Peña

Calderón

Piña

2019

RMxAA

Self Cite

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uvby − β photoelectric photometry of sixty-five stars in the direction of the open cluster NGC 1528 is presented. From the uvby − β photometry of the cluster we classified the spectral types of the stars which allowed us to determine the reddening (E(b-y) of 0.196 ± 0.054) and hence, their distance, in parsecs, of (954 ± 154). We determined membership of the stars to the cluster and the age (Log age equal 8.04) of the cluster. A metallicity [Fe/H] of −0.31 ± 0.08 was calculated.

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On the Nature of the Hads Star V2455 Cyg

Cited by 11 publications

References 11 publications

The Swift UVOT Stars Survey. III. Photometry and Color–Magnitude Diagrams of 103 Galactic Open Clusters

The Swift UVOT Stars Survey. III. Photometry and Color–Magnitude Diagrams of 103 Galactic Open Clusters

HD220735 and HD30110, new short period variable stars

STUDY OF THE OPEN CLUSTER NGC 1528 THROUGH uvby − β PHOTOELECTRIC PHOTOMETRY

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