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Register a new userThe open cluster King~1 in the second quadrant
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We analyse the poorly-studied open cluster King~1 in the second Galactic quadrant. From wide-field photometry we have studied the spatial distribution of this cluster. We determined that the centre of King~1 is located at $alpha_{2000}=00^{rm h}22^{rm m}$ and $delta_{2000}=+64degr23arcmin$. By parameterizing the stellar density with a King profile we have obtained a central density of $rho_{0}=6.5pm0.2$ star arcmin$^{-2}$ and a core radius of $r_{rm core}=1farcm9pm0farcm2$. By comparing the observed color-magnitude diagram of King~1 with those of similar open clusters and with different sets of isochrones, we have estimated an age of $2.8pm0.3$ Gyr, a distance modulus of $(m-M)_{rm o}=10.6pm0.1$ mag, and a reddening of $E(B-V)=0.80pm0.05$ mag. To complete our analysis we acquired medium resolution spectra for 189 stars in the area of King~1. From their derived radial velocities we determined an average velocity $leftlangle V_rrightrangle $=-53.1$pm$3.1 km s$^{-1}$. From the strength of the infrared mbox{Ca,{sc ii}} lines in red giants we have determined an average metallicity of $leftlangle [M/H]rightrangle$=+0.07$pm$0.08 dex. From spectral synthesis we have also estimated an $alpha$-elements abundance of $leftlangle [alpha/M]rightrangle$=-0.10$pm$0.08 dex.
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We present a UBV CCD photometric study of four open clusters, NGC 7245, King 9, IC 166 and King 13, located between $l = 90^o - 135^o$. All are embedded in a rich galactic field. NGC 7245 and King 9 are close together in the sky and have similar reddenings. The distances and ages are: NGC 7245, 3.8$pm$0.35 kpc and 400 Myr; King 9 (the most distant cluster in this quadrant) 7.9$pm$1.1 kpc and 3.0 Gyr. King 13 is 3.1$pm$0.3 kpc distant and 300 Myr old. King 9 and IC 166 (4.8$pm$0.5 kpc distant & 1 Gyr old) may be metal poor clusters (Z=0.008), as estimated from isochrone fitting. The average value of the distance of young clusters from the galactic plane in the above longitude range and beyond 2 kpc ($-47pm$16 pc, for 64 clusters), indicates that the young disk bends towards the southern latitudes.
Determining the distances to the Planck Galactic cold clumps (PGCCs) is crucial for the measurement of their physical parameters and the study of their Galactic distribution. Based on two large catalogues of stars with robust distances and reddening estimates from the literature, we have estimated accurate distances to 61 PGCCs in the second Galactic quadrant. For this purpose, we have selected stars along the sightlines overlapping with the cores of the sample clumps and fitted the reddening profiles with a simple reddening model. The typical uncertainties of the resultant distances of these PGCCs are less than 8 per cent. The new estimates differ significantly from the kinematic values, well known to suffer from large errors. With the new distances, we have updated the physical properties including the radii, masses and virial parameters of the cores of the PGCCs.
This paper presents an investigation of an old age open cluster King 11 using Gaias Early Data Release 3 (EDR3) data. Considering the stars with membership probability ($P_{mu}$) $> 90%$, we identified 676 most probable cluster members within the clusters limiting radius. The mean proper motion (PM) for King 11 is determined as: $mu_{x}=-3.391pm0.006$ and $mu_{y}=-0.660pm0.004$ mas yr$^{-1}$. The blue straggler stars (BSS) of King 11 show a centrally concentrated radial distribution. The values of limiting radius, age, and distance are determined as 18.51 arcmin, 3.63$pm$0.42 Gyr and $3.33pm0.15$ kpc, respectively. The clusters apex coordinates ($A=267.84^{circ} pm 1.01^{circ}$, $D=-27.48^{circ} pm 1.03^{circ}$) are determined using the apex diagram (AD) method and verified using the ($mu_U$,$mu_T$) diagram. We also obtained the orbit that the cluster follows in the Galaxy and estimated its tentative birthplace in the disk. The resulting spatial velocity of King 11 is 60.2 $pm$ 2.16 km s$^{-1}$. A significant oscillation along the $Z$-coordinate up to 0.556$pm$0.022~kpc is determined.
In this paper, we present astrophysical parameters of the open cluster King 13 based on the VI CCD and 2MASS JHKs photometric data. This is a poorly studied cluster, for which new results have been found in the present work. To identify probable members, we use proper motion data from Gaia DR2 catalogue. The mean proper motion of the cluster is determined as -2.8 pm 0.2 and -0.88 pm 0.14 mas yr{-1} and cluster extent is derived as 3.2. Using color-magnitude diagrams, we estimate the age and distance of the cluster as 510 pm 60 Myr and 3.84 pm 0.15 kpc respectively. Interstellar reddening E(B-V) in the direction of the cluster is determined as 0.80 pm 0.2 mag using color-color diagram. Mass function slope of the cluster is found to be comparable with the Salpeter value. The total mass of this cluster is derived as 270 M_{odot}. The present analysis shows that King 13 is a dynamically relaxed cluster.
Multi-color photometry of the stellar populations in five fields in the third Galactic quadrant centred on the clusters NGC 2215, NGC 2354, Haffner 22, Ruprecht 11, and ESO489SC01 is interpreted in terms of a warped and flared Galactic disk, without resort to an external entity such as the popular Monoceros or Canis Major overdensities. Except for NGC 2215, the clusters are poorly or unstudied previously. The data generate basic parameters for each cluster, including the distribution of stars along the line of sight. We use star counts and photometric analysis, without recourse to Galactic-model-based predictions or interpretations, and confirms earlier results for NGC 2215 and NGC 2354. ESO489SC01 is not a real cluster, while Haffner~22 is an overlooked cluster aged about 2.5 Gyr. Conclusions for Ruprecht~11 are preliminary, evidence for a cluster being marginal. Fields surrounding the clusters show signatures of young and intermediate-age stellar populations. The young population background to NGC~2354 and Ruprecht~11 lies 8-9 kpc from the Sun and $sim$1 kpc below the formal Galactic plane, tracing a portion of the Norma-Cygnus arm, challenging Galactic models that adopt a sharp cut-off of the disk 12-14 kpc from the Galactic center. The old population is metal poor with an age of 2-3 Gyr, resembling star clusters like Tombaugh 2 or NGC 2158. It has a large color spread and is difficult to locate precisely. Young and old populations follow a pattern that depends critically on the vertical location of the thin and/or thick disk, and whether or not a particular line of sight intersects one, both, or none.
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