The Cre/loxP recombination system for production of infectious mouse polyomavirus

Hron, Tomáš; Španielová, Hana; Suchanova, Jirina Zackova; Forstová, Jitka

doi:10.1016/j.virusres.2013.05.016

Cited by 7 publications

(11 citation statements)

References 21 publications

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“…The rotation curve described by OCs is similar to that derived from other thin disc populations such as Cepheids, H ii regions or molecular clouds (e.g. Hron 1987;Scott et al 1995;Glushkova et al 1998;Friel et al 2002b). It seems that the rotational velocity gradually decreases with age.…”

Section: Occaso Science Driverssupporting

confidence: 80%

The OCCASO survey: presentation and radial velocities of 12 Milky Way open clusters

Casamiquela

Carrera

Jordi

et al. 2016

Mon. Not. R. Astron. Soc.

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Open clusters (OCs) are crucial for studying the formation and evolution of the Galactic disc. However, the lack of a large number of OCs analyzed homogeneously hampers the investigations about chemical patterns and the existence of Galactocentric radial and vertical gradients, or an age-metallicity relation. To overcome this, we have designed the Open Cluster Chemical Abundances from Spanish Observatories survey (OCCASO). We aim to provide homogeneous radial velocities, physical parameters and individual chemical abundances of six or more Red Clump stars for a sample of 25 old and intermediate-age OCs visible from the Northern hemisphere. To do so, we use high resolution spectroscopic facilities (R 62, 000) available at Spanish observatories. We present the motivation, design and current status of the survey, together with the first data release of radial velocities for 77 stars in 12 OCs, which represents about 50% of the survey. We include clusters never studied with high-resolution spectroscopy before (NGC 1907, NGC 6991, NGC 7762), and clusters in common with other large spectroscopic surveys like the Gaia-ESO Survey (NGC 6705) and APOGEE (NGC 2682 and NGC 6819). We perform internal comparisons between instruments to evaluate and correct internal systematics of the results, and compare our radial velocities with previous determinations in the literature, when available. Finally, radial velocities for each cluster are used to perform a preliminar kinematic study in relation with the Galactic disc.

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Section: Occaso Science Driverssupporting

confidence: 80%

The OCCASO survey: presentation and radial velocities of 12 Milky Way open clusters

Casamiquela

Carrera

Jordi

et al. 2016

Mon. Not. R. Astron. Soc.

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“…In terms of the traditional characteristics used to categorize disk populations, the properties of the open clusters show overall consistency with those of the thin disk (Friel 1995). Their kinematics, and in particular the systemic rotational properties of the open cluster population, are very similar to those of the thin disk field stars and other disk tracers (Hron 1987;Scott et al 1995). Cluster ages, spatial distribution, and concentration to the Galactic plane are thin disk-like.…”

Section: Cluster N-capture Abundance Trends With R Gcmentioning

confidence: 81%

Zirconium, Barium, Lanthanum, and Europium Abundances in Open Clusters

Jacobson

Friel

2013

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We present an analysis of the s-process elements Zr, Ba, and La and the r-process element Eu in a sample of 50 stars in 19 open clusters. Stellar abundances of each element are based on measures of a minimum of two lines per species via both equivalent width and spectrum synthesis techniques. We investigate cluster mean neutron capture abundance trends as a function of cluster age and location in the Milky Way disk and compare them to results found in other studies in the literature. We find a statistically significant trend of increasing cluster [Ba/Fe] as a function of decreasing cluster age, in agreement with recent findings for other open cluster samples, supporting the increased importance of low mass AGB stars to the generation of s-process elements. However, the other s-process elements, [La/Fe] and [Zr/Fe] do not show similar dependences, in contrast to theoretical expectations and the limited observational data from other studies. Conversely, cluster [Eu/Fe] ratios show a slight increase with increasing cluster age, although with marginal statistical significance. Ratios of [s/r]-process abundances, [Ba/Eu] and [La/Eu], however, show more clearly the increasing efficiency of s-process relative to r-process enrichment in open cluster chemical evolution, with significant increases among younger clusters. Lastly, cluster neutron capture element abundances appear to be independent of Galactocentric distance. We conclude that a homogeneous analysis of a larger sample of open clusters is needed to resolve the apparent discrepant conclusions between different studies regarding s-process element abundance trends with age to better inform models of galactic chemical evolution.

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“…The most popular approach, the tangent-point method (e.g., Burton & Gordon 1978;Clemens 1985;Fich et al 1989;Sofue et al 2009;McClure-Griffiths & Dickey 2016), based on radio and mm observations of common molecules (Hi or CO), allows measuring the rotation curve within the solar orbit, although it is unreliable in the central regions of the Galaxy (Chemin et al 2015). The rotation curve outside the solar orbit can be measured with known distances and velocities of some tracers: H ii regions (Fich et al 1989;Brand & Blitz 1993), Cepheids (Pont et al 1994(Pont et al , 1997Metzger et al 1998;Kawata et al 2018), open clusters (Hron 1987), or planetary nebulae (Durand et al 1998), but the current uncertainties are considerable (see Figure 1 of Sofue et al 2009), mostly because of poorly known distances. Such approach is prone to systematic errors, as usually only one component of the velocity vector (radial or tangential) is known and the circular rotation is assumed.…”

Section: Introductionmentioning

confidence: 99%

Rotation Curve of the Milky Way from Classical Cepheids

Mróz

Udalski

Skowron

et al. 2019

ApJL

133

146

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Flat rotation curves of spiral galaxies are considered as an evidence for dark matter, but the rotation curve of the Milky Way is difficult to measure. Various objects were used to track the rotation curve in the outer parts of the Galaxy, but most studies rely on incomplete kinematical information and inaccurate distances. Here, we use a sample of 773 Classical Cepheids with precise distances based on mid-infrared period-luminosity relations coupled with proper motions and radial velocities from Gaia to construct the accurate rotation curve of the Milky Way up to the distance of ∼ 20 kpc from the Galactic center. We use a simple model of Galactic rotation to measure the rotation speed of the Sun Θ 0 = 233.6±2.8 km s −1 , assuming a prior on the distance to the Galactic center R 0 = 8.122±0.031 kpc from the Gravity Collaboration. The rotation curve at Galactocentric distances 4 R 20 kpc is nearly flat with a small gradient of −1.34 ± 0.21 km s −1 kpc −1 . This is the most accurate Galactic rotation curve at distances R > 12 kpc constructed so far.

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The Cre/loxP recombination system for production of infectious mouse polyomavirus

Cited by 7 publications

References 21 publications

The OCCASO survey: presentation and radial velocities of 12 Milky Way open clusters

The OCCASO survey: presentation and radial velocities of 12 Milky Way open clusters

Zirconium, Barium, Lanthanum, and Europium Abundances in Open Clusters

Rotation Curve of the Milky Way from Classical Cepheids

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