The low-mass pre-main sequence population of Scorpius OB1

Damiani, F.

doi:10.1051/0004-6361/201730960

Cited by 20 publications

(25 citation statements)

References 72 publications

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“…The volume of space investigated in this study is comparable with the dimensions of the nearby well-studied Scorpius-Centaurus (Sco-Cen) association. That region is composed of three main groups (Upper Scorpius, Upper Centaurus Lupus, and Lower Centaurus Crux Blaauw 1946;de Zeeuw et al 1999;Wright & Mamajek 2018;Damiani 2018) with ages from ∼5 to ∼20 Myr (e.g. Pecaut & Mamajek 2016).…”

Section: Discussionmentioning

confidence: 99%

“…More recently, the unprecedented quality of the astrometry provided by the second Gaia data release (Gaia DR2, Gaia Collaboration 2018b) has enabled detailed studies of the spatial and kinematic substructure of stellar associations within several hundreds of parsecs of the Sun (e.g. Kuhn et al 2019;Kounkel et al 2018;Damiani 2018;Karnath et al 2019;Zari et al 2018;Kos et al 2018).…”

Section: Introductionmentioning

confidence: 99%

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Expanding associations in the Vela-Puppis region

Cantat-Gaudin

Jordi

Wright

et al. 2019

A&A

112

113

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Context. The Vela-Puppis region is known to host the Vela OB2 association as well as several young clusters featuring OB and premain-sequence stars. Several spatial and kinematic subgroups have been identified in recent years. Aims. By grouping stars based on their positions and velocity, we can address the question of the dynamical history of the region and the mechanisms that drove stellar formation. The Gaia DR2 astrometry and photometry enables us to characterise the 3D spatial and 3D kinematic distribution of young stars and to estimate the ages of the identified components. Methods. We used an unsupervised classification method to group stars based on their proper motions and parallax. We studied the expansion rates of the different identified groups based on 3D velocities and on corrected tangential velocities. We used theoretical isochrones to estimate ages. Results. The young stars can be separated into seven main groups of different ages and kinematical distribution. All groups are found to be expanding, although the expansion is mostly not isotropic. Conclusions. The size of the region, the age substructure, and the anisotropic expansion rates are compatible with a prolonged period of star formation in a turbulent molecular cloud. The current kinematics of the stars cannot be explained by internal processes alone (such as gas expulsion). Key words. open clusters and associations: individual: Vela OB2 -open clusters and associations: individual: Trumpler 10open clusters and associations: individual: NGC 2547 -open clusters and associations: individual: NGC 2451Bstars: pre-main sequence Article published by EDP Sciences A17, page 1 of 18 A&A 626, A17 (2019)

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Expanding associations in the Vela-Puppis region

Cantat-Gaudin

Jordi

Wright

et al. 2019

A&A

112

113

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“…As it is known, in the color-color diagrams shown in Fig. 6, the intrinsic color-color locus is degenerate with respect to the reddening direction, except in the range of the Mtype stars (Damiani, 2018), where the intrinsic locus bends to- Fig. 6.…”

Section: Reddening Lawmentioning

confidence: 90%

“…Objects with infrared excess were identified by modeling their NIR/MIR SEDs as circumstellar dust in a disk or infalling envelope as done in Povich et al (2011). -parallaxes and proper motions from the Gaia DR2 catalog (Gaia Collaboration et al, 2016, 2018Lindegren et al, 2018).…”

Section: Gaia-eso Survey Spectroscopic Datamentioning

confidence: 99%

The Gaia-ESO Survey: Age spread in the star forming region NGC 6530 from the HR diagram and gravity indicators

Prisinzano

Damiani

Kalari

et al. 2019

A&A

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Context. In very young clusters, the stellar age distribution is the empirical proof of the duration of star cluster formation and thus it gives indications of the physical mechanisms involved in the star formation process. Determining the amount of interstellar extinction and the correct reddening law are crucial steps to derive fundamental stellar parameters and in particular accurate ages from the HR diagram. Aims. In this context, we derived accurate stellar ages for NGC 6530, the young cluster associated with the Lagoon Nebula to infer the star formation history of this region. Methods. We use the Gaia-ESO survey observations of the Lagoon Nebula, together with photometric literature data and Gaia DR2 kinematics, to derive cluster membership and fundamental stellar parameters. Using spectroscopic effective temperatures, we analyze the reddening properties of all objects and derive accurate stellar ages for cluster members. Results. We identified 652 confirmed and 9 probable members. The reddening inferred for members and non-members allows us to distinguish foreground objects, mainly main-sequence (MS) stars, and background objects, mainly giants. This classification is in agreement with the distances inferred from Gaia DR2 parallaxes for these objects. The foreground and background stars show a spatial pattern that allows us to trace the three-dimensional structure of the nebular dust component. Finally, we derive stellar ages for 382 confirmed cluster members for which we obtained the individual reddening values. In addition, we find that the gravity-sensitive γ index distribution for the M-type stars is correlated with stellar age. Conclusions. For all members with T eff < 5500 K, the mean logarithmic age is 5.84 (units of years) with a dispersion of 0.36 dex. The age distribution of stars with accretion and/or disk (CTTSe) is similar to that of stars without accretion and without disk (WTTSp). We interpret this dispersion as evidence of a real age spread since the total uncertainties on age determinations, derived from Monte Carlo simulations, are significantly smaller than the observed spread. This conclusion is supported by the evidence of a decreasing of the gravity-sensitive γ index as a function of stellar ages. The presence of a small age spread is also supported by the spatial distribution and the kinematics of old and young members. In particular, members with accretion and/or disk, formed in the last 1 Myr, show evidence of subclustering around the cluster center, in the Hourglass Nebula and in the M8-E region, suggesting a possible triggering of star formation events by the O-type star ionization fronts.

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“…The method of investigation examined in Damiani (2018) and successfully tested here to rederive the NGC 2264 cluster has an enormous potential for studies of young star clusters in the era of large-scale, homogeneous photometric surveys. Specifically, it can be readily implemented to statistically identify and map young distant (ě 1-2 kpc) clusters, that will become accessible for the first time with campaigns such as Pan-STARRS and LSST, and for which extensive spectroscopic surveys and X-ray surveys would not be feasible due to prohibitive integration times.…”

Section: Discussionmentioning

confidence: 99%

Deep, multiband photometry of low-mass stars to reveal young clusters: A blind study of the NGC2264 region

Venuti

Damiani

Prisinzano

2018

A&A

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Context. Thanks to their extensive and homogeneous sky coverage, deep, large-scale, multi-wavelength surveys are uniquely suited to statistically identify and map young star clusters in our Galaxy. Such studies are crucial to address themes like the initial mass function, or the modes and dynamics of star cluster formation and evolution. Aims. We aim to test a purely photometric approach to statistically identify a young clustered population embedded in a large population of field stars, with no prior knowledge on the nature of stars in the field. We conducted our blind test study on the NGC 2264 region, which hosts a well-known, richly populated young cluster ("3 Myr-old) and several active star-forming sites. Methods. We selected a large (4 deg 2 ) area around the NGC 2264 cluster, and assembled an extensive r, i, J catalog of the field from pre-existing large-scale surveys, notably Pan-STARRS1 and UKIDSS. We then mapped the stellar color locus on the (i´J, r´i) diagram to select M-type stars, which offer the following observational advantages with respect to more massive stars: i) they comprise a significant fraction of the Galactic stellar population; ii) their pre-main sequence phase lasts significantly longer than for higher-mass stars; iii) they exhibit the strongest luminosity evolution from the pre-main sequence to the main sequence; iv) their observed r, i, J colors provide a direct and empirical estimate of A V . A comparative analysis of the photometric and spatial properties of M-type stars as a function of A V enabled us to probe the structure and stellar content of our field. Results. Using only r, i, J photometry, we could identify two distinct populations in our field: a diffuse field population and a clustered population in the center of the field. The presence of a concentration of occulting material, spatially associated with the clustered population, allowed us to derive an estimate of its distance (800-900 pc) and age ("0.5-5 Myr); these values are overall consistent with the literature parameters for the NGC 2264 star-forming region. The extracted clustered population exhibits a hierarchical structure, with two main clumps and peaks in number density of objects around the most extincted locations within the field. An excellent agreement is found between the observed substructures for the clustered population and a map of the NGC 2264 subregions reported in the literature. Our selection of clustered members is coherent with the literature census of the NGC 2264 cluster for about 95% of the objects located in the inner regions of the field, where the estimated contamination rate by field stars in our sample is only 2%. In addition, the availability of a uniform dataset for a large area around the NGC 2264 region enabled us to discover a population of about a hundred stars with indications of statistical membership to the cluster, therefore extending the low-mass population census of NGC 2264 to distances of 10-15 pc from the cluster cores. Conclusions. By making use solely of deep, multi-band...

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The low-mass pre-main sequence population of Scorpius OB1

Cited by 20 publications

References 72 publications

Expanding associations in the Vela-Puppis region

Expanding associations in the Vela-Puppis region

The Gaia-ESO Survey: Age spread in the star forming region NGC 6530 from the HR diagram and gravity indicators

Deep, multiband photometry of low-mass stars to reveal young clusters: A blind study of the NGC2264 region

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