Anchors for the cosmic distance scale: the Cepheid QZ Normae in the open cluster NGC 6067

Majaess, D.; Sturch, Laura; Bidin, C. Moni; Soto, M.; Gieren, W.; Cohen, Roger E.; Mauro, F.; Geisler, D.; Bonatto, Charles Jose; Borissova, J.; Minniti, D.; Turner, D. G.; Lane, David J.; Madore, Barry F.; Carraro, G.; Бердников, Л. Н.

doi:10.1007/s10509-013-1495-1

Cited by 14 publications

(23 citation statements)

References 89 publications

(119 reference statements)

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“…All the stars observed in the present work are inside this radius. The Cepheid QZ Nor is located ≈ 20 arcmin from the cluster centre, and so it lies within the tidal radius upper limit, possibly in the halo, as suggested by previous works Majaess et al 2013;Anderson et al 2013). …”

Section: Centre and Cluster Radiussupporting

confidence: 82%

“…Mermilliod (1981b) estimated for this group a turnoff point at spectral type B6, as we have found for NGC 6067 in this work. Santos & Bica (1993) measuring the EW s of the Balmer lines and, more recently, Majaess et al (2013) using new BV JH and Padova isochrones obtained a similar value (log τ = 7.89 ± 0.15), even if the age of the Pleiades is now believed to be ≈ 120 Ma old. With an age just short of 100 Ma, NGC 6067 is the oldest cluster containing K0 -K2 Ib-II supergiants (see the discussion in Negueruela & Marco 2012).…”

Section: Fitting Isochronesmentioning

confidence: 73%

“…They have different pulsation periods (P ) inferred from well-studied light curves (Laney & Stobie 1994): V340 Nor is a fundamental mode pulsator (P = 11.30 d), whereas QZ Nor is an overtone mode pulsator (P = 3.78 d). According to these periods, Majaess et al (2013), by using different period-age relations (Efremov 2003;Bono et al 2005;Turner et al 2012), estimated the age of the Cepheids (see their table 1). The mean age of QZ Nor (89 ± 13 Ma) is in good agreement with that obtained in this work for the cluster.…”

Section: Cepheidsmentioning

confidence: 99%

“…Thus, the masses of the Cepheids, estimated with calibrations from models including the effect of rotation, are compatible with those expected for the cluster members. Unfortunately, the period evolution, which could greatly constrain their evolutionary stage, cannot be determined yet for these two Cepheids (Majaess et al 2013).…”

Section: Cepheidsmentioning

confidence: 99%

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NGC 6067: a young and massive open cluster with high metallicity

Alonso-Santiago

Negueruela

Marco

et al. 2017

Monthly Notices of the Royal Astronomical Society

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NGC 6067 is a young open cluster hosting the largest population of evolved stars among known Milky Way clusters in the 50 -150 Ma age range. It thus represents the best laboratory in our Galaxy to constrain the evolutionary tracks of 5 -7 M stars.We have used high-resolution spectra of a large sample of bright cluster members (45), combined with archival photometry, to obtain accurate parameters for the cluster as well as stellar atmospheric parameters. We derive a distance of 1.78 ± 0.12 kpc, an age of 90 ± 20 Ma and a tidal radius of 14.8 +6.8 −3.2 arcmin. We estimate an initial mass above 5 700 M , for a present-day evolved population of two Cepheids, two A supergiants and 12 red giants with masses ≈ 6 M .We also determine chemical abundances of Li, O, Na, Mg, Si, Ca, Ti, Ni, Rb, Y, and Ba for the red clump stars. We find a supersolar metallicity, [Fe/H]=+0.19±0.05, and a homogeneous chemical composition, consistent with the Galactic metallicity gradient. The presence of a Li-rich red giant, star 276 with A(Li)=2.41, is also detected. An over-abundance of Ba is found, supporting the enhanced s-process.The ratio of yellow to red giants is much smaller than one, in agreement with models with moderate overshooting, but the properties of the cluster Cepheids do not seem consistent with current Padova models for supersolar metallicity.

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Section: Centre and Cluster Radiussupporting

confidence: 82%

Section: Fitting Isochronesmentioning

confidence: 73%

Section: Cepheidsmentioning

confidence: 99%

Section: Cepheidsmentioning

confidence: 99%

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NGC 6067: a young and massive open cluster with high metallicity

Alonso-Santiago

Negueruela

Marco

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…So, we also spectroscopically analyzed XZ CMa to confirm or exclude the cluster membership. In fact, cluster Cepheids are important to fixing the distance scale (see, e.g., Majaess et al 2013aMajaess et al , 2013b.…”

Section: Tombaugh1: Backgroundmentioning

confidence: 99%

PROPERTIES OF THE OPEN CLUSTER TOMBAUGH 1 FROM HIGH-RESOLUTION SPECTROSCOPY AND uvbyCaHβ PHOTOMETRY*

Silva

Carraro²,

Anthony-Twarog

et al. 2015

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Open clusters can be the key to deepening our knowledge on various issues involving the structure and evolution of the Galactic disk and details of stellar evolution because a cluster's properties are applicable to all its members. However, the number of open clusters with detailed analysis from high-resolution spectroscopy or precision photometry imposes severe limitations on studies of these objects. To expand the number of open clusters with well-defined chemical abundances and fundamental parameters, we investigate the poorly studied, anticenter open cluster Tombaugh 1. Using precision uvbyCaHβ photometry and high-resolution spectroscopy, we derive the cluster's reddening, obtain photometric metallicity estimates, and, for the first time, present a detailed abundance analysis of 10 potential cluster stars (nine clump stars and one Cepheid). Using the radial position from the cluster center and multiple color indices, we have isolated a sample of unevolved, probable single-star members of Tombaugh 1. From 51 stars, the cluster reddening is found to be -.008, where the errors refer to the internal standard errors of the mean. The weighted photometric metallicity from m 1 and hk is [Fe/H]=−0.10±0.02, while a match to the Victoria-Regina Strömgren isochrones leads to an age of 0.95±0.10 Gyr and an apparent modulus of -m M ( )=13.10±0.10. Radial velocities identify six giants as probable cluster members, and the elemental abundances of Fe, Na, Mg, Al, Si, Ca, Ti, Cr, Ni, Y, Ba, Ce, and Nd have been derived for both the cluster and the field stars. Tombaugh 1 appears to be a typical inner thin disk, intermediate-age open cluster of slightly subsolar metallicity, located just beyond the solar circle, with solar elemental abundance ratios except for the heavy s-process elements, which are a factor of two above solar. Its metallicity is consistent with a steep metallicity gradient in the galactocentric region between 9.5 and 12 kpc. Our study also shows that Cepheid XZ CMa is not a member of Tombaugh 1 and reveals that this Cepheid presents signs of barium enrichment, making it a probable binary star.

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A high-mass planetary nebula in a Galactic open cluster

et al. 2019

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Planetary Nebulae are the ionised ejected envelopes surrounding the remnant cores of dying stars. Theory predicts that main-sequence stars with one to about eight times the mass of our sun may eventually form planetary nebulae. Until now no example has been confirmed at the higher mass range. Here we report that planetary nebula BMP J1613-5406 is associated with Galactic star cluster NGC 6067. Stars evolving off the main sequence of this cluster have a mass around five solar masses. Confidence in the planetary nebula-cluster association comes from their tightly consistent radial velocities in a sightline with a steep velocity-distance gradient, common distances, reddening and location of the planetary nebula within the cluster boundary. This is an unprecedented example of a planetary nebular whose progenitor star mass is getting close to the theoretical lower limit of core-collapse supernova formation. It provides evidence supporting theoretical predictions that 5+ solar mass stars can form planetary nebulae. Further study should provide fresh insights into stellar and Galactic chemical evolution. Introduction and Background Stars live their lives as nuclear fusion reactors and their fate usually depends on birth mass. Massive stars burn their fuel quickly and can explode as supernovae after a few million years. The vast majority of stars have lower mass and live for many billions of years. Planetary Nebulae (PNe) may eventually form from stars of ~1-8 Mʘ. Such PNe progenitors represent 90% of all stars more massive than the sun. Towards the end of their lives most such stars pass through the Asymptotic Giant Branch (AGB) phase where the bulk of mass-loss occurs. A final, ejected envelope is ionized by the UV radiation field from the hot, remnant central star (CS) forming a

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Anchors for the cosmic distance scale: the Cepheid QZ Normae in the open cluster NGC 6067

Cited by 14 publications

References 89 publications

NGC 6067: a young and massive open cluster with high metallicity

NGC 6067: a young and massive open cluster with high metallicity

PROPERTIES OF THE OPEN CLUSTER TOMBAUGH 1 FROM HIGH-RESOLUTION SPECTROSCOPY AND uvbyCaHβ PHOTOMETRY*

A high-mass planetary nebula in a Galactic open cluster

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