New Cepheid variables in the young open clusters Berkeley 51 and Berkeley 55

Lohr, M. E.; Negueruela, I.; Tabernero, H. M.; Clark, J. S.; Lewis, Fraser; Roche, P.

doi:10.1093/mnras/sty1280

Cited by 11 publications

(12 citation statements)

References 31 publications

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“…Recently, Lindegren et al (2018) reported a general offset in Gaia parallaxes by -0.029 mas though there is also some evidence that the offset increases for the distances larger than 1 kpc (Stassun & Torres 2018;Lohr et al 2018). This has been further confirmed by many other surveys although with slightly different values (e.g., Schönrich et al 2019;Zinn et al 2019).…”

Section: Parallax Criteria On Membership Selectionmentioning

confidence: 98%

Photometric, kinematic, and variability study in the young open cluster NGC 1960

Joshi

Maurya

John

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a comprehensive photometric analysis of a young open cluster NGC 1960 (= M36) along with the long-term variability study of this cluster. Based on the kinematic data of Gaia DR2, the membership probabilities of 3871 stars are ascertained in the cluster field among which 262 stars are found to be cluster members. Considering the kinematic and trigonometric measurements of the cluster members, we estimate a mean cluster parallax of 0.86±0.05 mas and mean proper motions of µ RA = -0.143±0.008 mas yr −1 , µ Dec = -3.395±0.008 mas yr −1 . We obtain basic parameters of the cluster such as E(B − V) = 0.24±0.02 mag, log(Age/yr)=7.44±0.02, and d = 1.17±0.06 kpc. The mass function slope in the cluster for the stars in the mass range of 0.72-7.32 M ⊙ is found to be γ = -1.26±0.19. We find that mass segregation is still taking place in the cluster which is yet to be dynamically relaxed. This work also presents first high-precision variability survey in the central 13 ′ × 13 ′ region of the cluster. The V band photometric data accumulated on 43 nights over a period of more than 3 years reveals 76 variable stars among which 72 are periodic variables. Among them, 59 are short-period (P < 1 day)and 13 are long-period (P > 1 day). The variable stars have V magnitudes ranging between 9.1 to 19.4 mag and periods between 41 minutes to 10.74 days. On the basis of their locations in the H-R diagram, periods and characteristic light curves, the 20 periodic variables belong to the cluster. We classified them as 2 δ-Scuti, 3 γ-Dor, 2 slowly pulsating B stars, 5 rotational variables, 2 non-pulsating B stars and 6 as miscellaneous variables.

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Section: Parallax Criteria On Membership Selectionmentioning

confidence: 98%

Photometric, kinematic, and variability study in the young open cluster NGC 1960

Joshi

Maurya

John

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…It has already been employed in many astrophysical contexts, including the study of stars in open clusters 6, but for the TiO γ and bands. (Lohr et al 2018;Alonso-Santiago et al 2019), stars in galaxies of the Local Group (Tabernero et al 2018), and exoplanet host stars (Borsa et al 2021;Demangeon et al 2021).…”

Section: Steparsynmentioning

confidence: 99%

The CARMENES search for exoplanets around M dwarfs. Stellar atmospheric parameters of target stars with SteParSyn

Marfil,

Tabernero,

Montes

et al. 2021

Preprint

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We determined effective temperatures, surface gravities, and metallicities for a sample of 343 M dwarfs observed with CARMENES, the double-channel, high-resolution spectrograph installed at the 3.5 m telescope at Calar Alto Observatory. We employed SteParSyn, a Bayesian spectral synthesis implementation particularly designed to infer the stellar atmospheric parameters of late-type stars following a Markov chain Monte Carlo approach. We made use of the BT-Settl model atmospheres and the radiative transfer code turbospectrum to compute a grid of synthetic spectra around 75 magnetically insensitive Fe i and Ti i lines plus the TiO γ and bands. To avoid any potential degeneracy in the parameter space, we imposed Bayesian priors on T eff and log g based on the comprehensive, multi-band photometric data available for the sample. We find that this methodology is suitable down to M7.0 V, where refractory metals such as Ti are expected to condense in the stellar photospheres. The derived T eff , log g, and [Fe/H] range from 3000 to 4200 K, 4.5 to 5.3 dex, and −0.7 to 0.2 dex, respectively. Although our T eff scale is in good agreement with the literature, we report large discrepancies in the [Fe/H] scales, which might arise from the different methodologies and sets of lines considered. However, our [Fe/H] is in agreement with the metallicity distribution of FGK-type stars in the solar neighbourhood and correlates well with the kinematic membership of the targets in the Galactic populations. Lastly, excellent agreement in T eff is found for M dwarfs with interferometric angular diameter measurements, as well as in the [Fe/H] between the components in the wide physical FGK+M and M+M systems included in our sample.

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“…Combos for which we obtain 𝑃( 𝐴|𝐵) > 0.01 and that appear at least once in Turner's database, A13 (with membership probability > 0.10 from their work), or Chen, de Grĳs, & Deng (2015), together with the spectroscopically confirmed cluster Cepheids described by Lohr et al (2018) and Clark et al (2015), and the association recently found by Negueruela, Dorda, & Marco (2020), are listed at the top of Table A2 (19 in total).…”

Section: Gq Vul and Fsr 0158mentioning

confidence: 90%

“…We rely for this on the cross-survey validation performed by the OGLE team, which also includes targets from the Asteroid Terrestrial-impact Last Alert System survey (ATLAS, Heinze et al 2018) and the All Sky Automated Survey for Supernovae (ASAS-SN, Jayasinghe et al 2018Jayasinghe et al , 2019a surveys. The Cepheids discovered by Clark et al (2015) in the cluster BH 222 and by Lohr et al (2018)…”

Section: Cepheids Samplementioning

confidence: 99%

“…In spite of their importance, only a small number of bona fide classical Cepheids in open clusters has been reported so far. The available literature illustrates the numerous attempts to increase the list of reliable cluster-Cepheid pairs, starting with the identification of the Cepheids S Nor and U Sgr as members of NGC 6087 and M 25, respectively (Irwin 1955), and extending throughout the last decades (e.g., van den Bergh 1957;Kraft 1962;Efremov 1964;Turner 1986;Turner, Forbes, & Pedreros 1992;Turner et al 1998b;Baumgardt, Dettbarn, & Wielen 2000;Hoyle, Shanks, & Tanvir 2003;Turner et al 2005;An, Terndrup, & Pinsonneault 2007;Majaess, Turner, & Lane 2008;Turner et al 2008;Turner 2010;Anderson, Eyer, & Mowlavi 2013;Chen, de Grĳs, & Deng 2015;Lohr et al 2018;Negueruela, Dorda, & Marco 2020). These studies have provided the approximately two tens of currently identified cluster Cepheids.…”

Section: Introductionmentioning

confidence: 99%

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A revisited study of Cepheids in open clusters in the Gaia era

Medina,

Lemasle,

Grebel

2021

Preprint

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In this paper we revisit the problem of identifying bona fide cluster Cepheids by performing an all-sky search for Cepheids associated with open clusters and making use of state-of-the-art catalogued information for both Cepheids and clusters, based on the unparalleled astrometric precision of the second and early third data releases of the Gaia satellite. We determine membership probabilities by following a Bayesian approach using spatial and kinematic information of the potential cluster-Cepheid pairs. We confirm 19 Cepheid-cluster associations considered in previous studies as bona-fide, and question the established cluster membership of six other associations. In addition, we identify 138 cluster Cepheid candidates of potential interest, mostly in recently discovered open clusters. We report on at least two new clusters possibly hosting more than one Cepheid. Furthermore, we explore the feasibility of using open clusters hosting Cepheids to empirically determine the Cepheid period-age relation through the use of Gaia and 2MASS photometry and a semi-automated method to derive cluster ages. We conclude that the usage of cluster Cepheids as tentative probes of the period-age relations still faces difficulties due to the sparsely populated red giant branch and the stochastically sampled main-sequence turn-off of the open clusters, making age determinations a challenging task. This biases the age-dateable cluster selection for Cepheid period-age studies towards older and high-mass clusters.

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New Cepheid variables in the young open clusters Berkeley 51 and Berkeley 55

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Cited by 11 publications

References 31 publications

Photometric, kinematic, and variability study in the young open cluster NGC 1960

Photometric, kinematic, and variability study in the young open cluster NGC 1960

The CARMENES search for exoplanets around M dwarfs. Stellar atmospheric parameters of target stars with SteParSyn

A revisited study of Cepheids in open clusters in the Gaia era

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