Notes on the open cluster NGC 1252 with the variable carbon star TW Horologii as a probable member

Bouchet, P.; Thé, P.S.

doi:10.1086/131195

Cited by 9 publications

(7 citation statements)

References 6 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The photometry confirms that NGC 1901 is a physical system which is also supported by proper motions. For NGC 1252 we describe a different set of stars as compared to the object interpreted by Bouchet & Thé (1983), and questioned by Eggen (1984) and Baumgardt (1998). The present CMD suggests a TO and MS, so that a physical stellar group cannot be ruled out.…”

Section: Discussionmentioning

confidence: 70%

See 1 more Smart Citation

Open clusters or their remnants: $\vec{B}$ and $\vec{V}$ photometry of NGC 1901 and NGC 1252

Pavani

Bica

Dutra

et al. 2001

A&A

View full text Add to dashboard Cite

Abstract. Photometry in the B and V bands is presented for the southern stellar groups NGC 1901 and NGC 1252. NGC 1901 is often described as an open cluster while NGC 1252 consists of a concentration of about 20 stars centered ≈20 north of the original New General Catalogue coordinates, and at the southwest edge of the large region previously assigned to this object in the literature. NGC 1901 has a clear main sequence and shares similarities with the Hyades. We derive a reddening value E(B −V ) = 0.04, a distance from the Sun d = 0.45 kpc (Z = −0.23 kpc) and an age 0.6 ± 0.1 Gyr. NGC 1901 is conclusively a physical system, dynamically comparable to or more evolved than the Hyades. The colour-magnitude diagram of NGC 1252 suggests a turnoff and main sequence, and a total of 12 probable members. We simulated the Galactic field colour-magnitude diagram in the same direction and found it to be a poor match to NGC 1252, suggesting that NGC 1252 is not a field fluctuation. Isochrone fitting to the probable members is consistent with E(B − V ) = 0.02, d = 0.64 kpc (Z = −0.46 kpc) and an age 3 ± 1 Gyr. NGC 1252 cannot be ruled out as a physical group with the available data. If so, evidence is found that it is not a classical open cluster, but rather an open cluster remnant.

show abstract

Section: Discussionmentioning

confidence: 70%

“…NGC 1252 was discussed in Bica et al (2001), who refer to a stellar concentration at the southwest edge of Bouchet & Thé's (1983) definition of NGC 1252, which is a sparse collection of stars in a much larger field. NGC 1252 is described in the NGC as a star cluster containing 18 or 20 stars.…”

Section: Introductionmentioning

confidence: 99%

Open clusters or their remnants: $\vec{B}$ and $\vec{V}$ photometry of NGC 1901 and NGC 1252

Pavani

Bica

Dutra

et al. 2001

A&A

View full text Add to dashboard Cite

show abstract

“…In this instance, the BSS is not much brighter than the turnoff, the overwhelming effect of the BSS is completely due to the under-abundant cluster members. Meanwhile, a B9.5 V star is identified as the only confirmed member BSS in NGC 1252, based on the photometric study by Bouchet & The (1983). It suffers the same problem as that on Tombaugh 1 on having very small numbers of both N BS and N 2 (see Table 1).…”

Section: Tombaugh 1 and Ngc 1252mentioning

confidence: 97%

Blue Stragglers in Galactic Open Clusters and Integrated Spectral Energy Distributions

Xin

Deng

2005

ApJ

View full text Add to dashboard Cite

Synthetic integrated spectral properties of the old Galactic open clusters are studies in this work, where twenty-seven Galactic open clusters of ages ≥ 1Gyr are selected as the working sample. Based on the photometric observations of these open clusters, synthetic integrated spectrum has been made for the stellar population of each cluster. The effects of blue straggler stars (BSSs) on the conventional simple stellar population (SSP) model are analyzed on an individual cluster base. It is shown that the BSSs, whose holding positions in the color-magnitude diagrams (CMDs) cannot be predicted by the current single-star evolution theory, present significant modifications to the integrated properties of theoretical SSP model. The synthesized integrated spectral energy distributions (ISEDs) of our sample clusters are dramatically different from the SSPs based on isochrone only. The BSSs corrected ISEDs of stellar populations show systematic enhancements towards shorter wavelength in the spectra. When measured with wide-band colors in unresolvable conditions, the age of a stellar population can be seriously under-estimated by the conventional SSP model. Therefore, considering the common existence of BSS component in real stellar populations, a considerable amount of alternations on the conventional ISEDs should be expected when applying the technique of evolutionary population synthesis (EPS) to more complicated stellar systems.

show abstract

“…Appendix A.1: NGC 1252 marked this object as unverified in the Revised NGC. Bouchet & The (1983) mention that it is 'difficult to decide whether the cluster is real' but also list 14 possible members. Eggen (1984) considered the existence of this object unlikely and Baumgardt (1998) made use of Hipparcos data to conclude that NGC 1252 does not exist.…”

Section: Appendix A: Notes On Individual Asterismsmentioning

confidence: 99%

Clusters and mirages: cataloguing stellar aggregates in the Milky Way

Cantat-Gaudin

Anders

2020

A&A

245

View full text Add to dashboard Cite

Context.Many of the open clusters listed in modern catalogues were initially reported by visual astronomers as apparent overdensities of bright stars. As observational techniques and analysis methods continue to improve, some of them have been shown to be chance alignments of stars and not true clusters. Recent publications making use of Gaia DR2 data have provided membership lists for over a thousand clusters, however, many nearby objects listed in the literature have so far evaded detection. Aims. We aim to update the Gaia DR2 cluster census by performing membership determinations for known clusters that had been missed by previous studies and for recently-discovered clusters. We investigate a sub-set of non-detected clusters that, according to their literature parameters, should be easily visible in Gaia. Confirming or disproving the existence of old, inner-disc, high-altitude clusters is especially important as their survival or disruption is linked to the dynamical processes that drive the evolution of the Milky Way. Methods. We employed the Gaia DR2 catalogue and a membership assignment procedure, as well as visual inspections of spatial, proper motion, and parallax distributions. We used membership lists provided by other authors when available. Results. We derived membership lists for 150 objects, including ten that were already known prior to Gaia. We compiled a final list of members for 1481 clusters. Among the objects that we are still unable to identify with the Gaia data, we argue that many (mostly putatively old, relatively nearby, high-altitude objects) are not true clusters. Conclusions. At present, the only confirmed cluster located further than 500 pc away from the Galactic plane within the Solar circle is NGC 6791. It is likely that the objects discussed in this study only represent a fraction of the non-physical groupings erroneously listed in the catalogues as genuine open clusters and that those lists need further cleaning.

show abstract

Notes on the open cluster NGC 1252 with the variable carbon star TW Horologii as a probable member

Cited by 9 publications

References 6 publications

Open clusters or their remnants: $\vec{B}$ and $\vec{V}$ photometry of NGC 1901 and NGC 1252

Open clusters or their remnants: $\vec{B}$ and $\vec{V}$ photometry of NGC 1901 and NGC 1252

Blue Stragglers in Galactic Open Clusters and Integrated Spectral Energy Distributions

Clusters and mirages: cataloguing stellar aggregates in the Milky Way

Contact Info

Product

Resources

About