The old anticentre open cluster Berkeley 32: Membership and fundamental parameters

V. D&apos;Orazi; A. Bragaglia; M. Tosi; L. Di Fabrizio; E. V. Held

doi:10.1111/j.1365-2966.2006.10118.x

The old anticentre open cluster Berkeley 32: Membership and fundamental parameters

V. D'Orazi^*, A. Bragaglia, M. Tosi, L. Di Fabrizio, E. V. Held

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

12 Citations (Scopus)

Abstract

We have obtained medium- and low-resolution spectroscopy and BVI CCD imaging of Berkeley 32, an old open cluster which lies in the anticentre direction. From the radial velocities of 48 stars in the cluster direction, we found that 31 of them, in crucial evolutionary phases, are probable cluster members, with an average radial velocity of + 106.7 (σ = 8.5) km s ^-1. From isochrone fitting to the colour-magnitude diagrams of Berkeley 32, we have obtained an age of 6.3 Gyr, (m - M) ₀ = 12.48 and E(B - V) = 0.10. The best fit is obtained with Z = 0.008. A consistent distance, (m - M) ₀ ≃ 12.6 ± 0.1, has been derived from the mean magnitude of red clump stars with confirmed membership; we may assume (m - M) ₀ ≃ 12.55 ± 0.1. The colour-magnitude diagram of the nearby field observed to check for field stars contamination looks intriguingly similar to that of the Canis Major overdensity.

Original language	English
Pages (from-to)	471-478
Number of pages	8
Journal	Monthly Notices of the Royal Astronomical Society
Volume	368
Issue number	1
DOIs	https://doi.org/10.1111/j.1365-2966.2006.10118.x
Publication status	Published - May 2006
Externally published	Yes

Keywords

Hertzsprung-Russell (HR) diagram
Open clusters and associations: general
Open clusters and associations: individual: Berkeley 32

Access to Document

10.1111/j.1365-2966.2006.10118.x

Cite this

@article{d67df2c8ac7e41369d2b0b204e208bbf,

title = "The old anticentre open cluster Berkeley 32: Membership and fundamental parameters",

abstract = "We have obtained medium- and low-resolution spectroscopy and BVI CCD imaging of Berkeley 32, an old open cluster which lies in the anticentre direction. From the radial velocities of 48 stars in the cluster direction, we found that 31 of them, in crucial evolutionary phases, are probable cluster members, with an average radial velocity of + 106.7 (σ = 8.5) km s -1. From isochrone fitting to the colour-magnitude diagrams of Berkeley 32, we have obtained an age of 6.3 Gyr, (m - M) 0 = 12.48 and E(B - V) = 0.10. The best fit is obtained with Z = 0.008. A consistent distance, (m - M) 0 ≃ 12.6 ± 0.1, has been derived from the mean magnitude of red clump stars with confirmed membership; we may assume (m - M) 0 ≃ 12.55 ± 0.1. The colour-magnitude diagram of the nearby field observed to check for field stars contamination looks intriguingly similar to that of the Canis Major overdensity.",

keywords = "Hertzsprung-Russell (HR) diagram, Open clusters and associations: general, Open clusters and associations: individual: Berkeley 32",

author = "V. D'Orazi and A. Bragaglia and M. Tosi and {Di Fabrizio}, L. and Held, {E. V.}",

year = "2006",

month = may,

doi = "10.1111/j.1365-2966.2006.10118.x",

language = "English",

volume = "368",

pages = "471--478",

journal = "Monthly Notices of the Royal Astronomical Society: Letters",

issn = "1745-3925",

publisher = "Oxford University Press",

number = "1",

}

TY - JOUR

T1 - The old anticentre open cluster Berkeley 32

T2 - Membership and fundamental parameters

AU - D'Orazi, V.

AU - Bragaglia, A.

AU - Tosi, M.

AU - Di Fabrizio, L.

AU - Held, E. V.

PY - 2006/5

Y1 - 2006/5

N2 - We have obtained medium- and low-resolution spectroscopy and BVI CCD imaging of Berkeley 32, an old open cluster which lies in the anticentre direction. From the radial velocities of 48 stars in the cluster direction, we found that 31 of them, in crucial evolutionary phases, are probable cluster members, with an average radial velocity of + 106.7 (σ = 8.5) km s -1. From isochrone fitting to the colour-magnitude diagrams of Berkeley 32, we have obtained an age of 6.3 Gyr, (m - M) 0 = 12.48 and E(B - V) = 0.10. The best fit is obtained with Z = 0.008. A consistent distance, (m - M) 0 ≃ 12.6 ± 0.1, has been derived from the mean magnitude of red clump stars with confirmed membership; we may assume (m - M) 0 ≃ 12.55 ± 0.1. The colour-magnitude diagram of the nearby field observed to check for field stars contamination looks intriguingly similar to that of the Canis Major overdensity.

AB - We have obtained medium- and low-resolution spectroscopy and BVI CCD imaging of Berkeley 32, an old open cluster which lies in the anticentre direction. From the radial velocities of 48 stars in the cluster direction, we found that 31 of them, in crucial evolutionary phases, are probable cluster members, with an average radial velocity of + 106.7 (σ = 8.5) km s -1. From isochrone fitting to the colour-magnitude diagrams of Berkeley 32, we have obtained an age of 6.3 Gyr, (m - M) 0 = 12.48 and E(B - V) = 0.10. The best fit is obtained with Z = 0.008. A consistent distance, (m - M) 0 ≃ 12.6 ± 0.1, has been derived from the mean magnitude of red clump stars with confirmed membership; we may assume (m - M) 0 ≃ 12.55 ± 0.1. The colour-magnitude diagram of the nearby field observed to check for field stars contamination looks intriguingly similar to that of the Canis Major overdensity.

KW - Hertzsprung-Russell (HR) diagram

KW - Open clusters and associations: general

KW - Open clusters and associations: individual: Berkeley 32

UR - http://www.scopus.com/inward/record.url?scp=33645838607&partnerID=8YFLogxK

U2 - 10.1111/j.1365-2966.2006.10118.x

DO - 10.1111/j.1365-2966.2006.10118.x

M3 - Article

AN - SCOPUS:33645838607

VL - 368

SP - 471

EP - 478

JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

SN - 1745-3925

IS - 1

ER -

The old anticentre open cluster Berkeley 32: Membership and fundamental parameters

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Cite this