Detection of new O-type stars in the obscured stellar cluster Tr 16-SE in the Carina Nebula with KMOS

Preibisch, Thomas; Flaischlen, S.; Göppl, Christiane; Ercolano, Barbara; Roccatagliata, V.

doi:10.1051/0004-6361/202039620

Cited by 9 publications

(20 citation statements)

References 46 publications

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“…Not being a true cluster, Villafranca O-025 does not show a central concentration and the limits traditionally assigned to Trumpler 16 are established actually by the V-shaped dust lane immediately to its south, which is placed in the foreground with respect to the Carina nebula (top left plot in Fig. 7 of Maíz Apellániz & Barbá 2018, see also Preibisch et al 2021). Nevertheless, the stellar population of Villafranca O-025 is relatively easy to identify thanks to its richness and to its relatively low extinction in comparison with the background stars.…”

Section: Villafranca O-025 = Trumpler 16 Ementioning

confidence: 94%

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The Villafranca catalog of Galactic OB groups

Apellániz

Barbá

Aranda

et al. 2022

A&A

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Context. This is the second paper of a series on Galactic OB groups that uses astrometric and photometric data from Gaia and spectral classifications from the Galactic O-Star Spectroscopic Survey (GOSSS) and the Library of Libraries of Massive-star high-Resolution spectra (LiLiMaRlin). The previous paper was based on the second Gaia data release (DR2). Since then, the early third Gaia data release (EDR3) has appeared with new astrometry and photometry. Aims. The two aims of this paper are to revise the results for the sample from paper I using Gaia EDR3 data and to expand the sample of analyzed stellar groups to 26, from Villafranca O-001 to Villafranca O-026. Methods. We used GOSSS to select Galactic stellar groups with O stars and an updated version of the method in paper 0 of this series, combining Gaia EDR3 G + G BP + G RP photometry, positions, proper motions, and parallaxes to assign memberships and measure distances. We present 99 spectra from GOSSS and 32 from LiLiMaRlin for stars in the analyzed groups or in their foreground.Results. We derived distances to the 26 stellar groups with unprecedented precision and accuracy, with total (random plus systematic) uncertainties lower than 1% for distances within 1 kpc and of ∼3% around 3 kpc, which are values almost four times better than for Gaia DR2. We provide homogeneous spectral types for 110 stars and correct a number of errors in the literature, especially for objects in Villafranca O-023 (Orion nebula cluster). For each group, we discuss its membership and present possible runaway and walkaway stars. At least two of the studied groups, Villafranca O-O12 S in NGC 2467 and Villafranca O-014 NW in the North America nebula, are orphan clusters in which the most massive stars have been ejected by dynamical interactions, leaving objects with a capped mass function. The existence of such clusters has important consequences for the study of the initial mass function (IMF), the distribution of supernova explosions across the Galaxy, and the population and dynamics of isolated compact objects. We fit pre-main-sequence (PMS) isochrones to the color-magnitude diagrams (CMDs) of four clusters to derive ages of 2.0±0.5 Ma for Villafranca O-026 (σ Orionis cluster), 4±2 Ma for Villafranca O-016 (NGC 2264), 5.0±0.5 Ma for Villafranca O-021 (NGC 2362), and 8±2 Ma for Villafranca O-024 (γ Velorum cluster).

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Section: Villafranca O-025 = Trumpler 16 Ementioning

confidence: 94%

“…The census should be complete in the region barring the unknown classification of η Car B and (unlikely) objects hidden by large extinction and source confusion(Smith 2006a;Preibisch et al 2021). …”

mentioning

confidence: 99%

The Villafranca catalog of Galactic OB groups

Apellániz

Barbá

Aranda

et al. 2022

A&A

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“…IMPS with spectral types G through early K are the progenitors of zero-age main-sequence (ZAMS) late-B through A-type stars. Fully radiative AB stars possess neither magnetic dynamos nor sufficiently strong winds to power the shock-driven X-rays commonly observed from massive, O-and early-B-type stars (Gagné et al 2011;Nazé et al 2011;Preibisch et al 2021). This implies that any intrinsic X-ray emission from convective IMPS should disappear over timescales shorter than the <10 Myr ZAMS arrival times of >2M e stars (Siess et al 2000;Haemmerlé et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Characterizing the X-Ray Emission of Intermediate-mass Pre-main-sequence Stars

Nuñez

Povich

Binder

et al. 2021

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We use X-ray and infrared observations to study the properties of three classes of young stars in the Carina Nebula: intermediate-mass (2-5 M e ) pre-main-sequence stars (IMPS; i.e., intermediate-mass T Tauri stars), late-B and A stars on the zero-age main sequence (AB), and lower-mass T Tauri stars (TTS). We divide our sources among these three subclassifications and further identify disk-bearing young stellar objects versus diskless sources with no detectable infrared (IR) excess emission using IR (1-8 μm) spectral energy distribution modeling. We then perform X-ray spectral fitting to determine the hydrogen-absorbing column density (N H ), absorption-corrected X-ray luminosity (L X ), and coronal plasma temperature (kT) for each source. We find that the X-ray spectra of both IMPS and TTS are characterized by similar kT and N H , and on average L X /L bol ∼4×10 −4 . IMPS are systematically more luminous in X-rays (by ∼0.3 dex) than all other subclassifications, with median L X =2.5×10 31 erg s −1 , while AB stars of similar masses have X-ray emission consistent with TTS companions. These lines of evidence converge on a magnetocoronal flaring source for IMPS X-ray emission, a scaled-up version of the TTS emission mechanism. IMPS therefore provide powerful probes of isochronal ages for the first ∼10 Myr in the evolution of a massive stellar population, because their intrinsic, coronal X-ray emission decays rapidly after they commence evolving along radiative tracks. We suggest that the most luminous (in both X-rays and IR) IMPS could be used to place empirical constraints on the location of the intermediate-mass stellar birth line.

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“…This sample was complemented by 15 additional OB stars in the Carina Nebula listed in Shull et al (2021). We also added 8 OB stars which were recently identified in the cluster Tr16-SE (Preibisch et al 2021), the 5 OB stars known in NGC 3324 (see Preibisch et al 2014a), and 99 B stars from NGC 3293 (Evans et al 2005). This results in a sample of 241 OB stars in the CNC.…”

Section: Construction Of the Ob Star Samplementioning

confidence: 99%

“…A study of the Gaia EDR3 data for 69 massive stars in the central Carina Nebula by Shull et al (2021) found a common distance of (2.35 ± 0.08) kpc for these stars and no significant differences in the distances of the central Carina Nebula clusters Tr 14, 15, and 16. As pointed out by the authors, the controversy over the 1 A good example for the strong spatial variations of cloud extinction in the Carina Nebula is the highly obscured cluster Tr 16-SE (see Preibisch et al 2021): the stars in Tr 16-SE suffer extinctions of A V > ∼ 5 − 10 mag, making them very faint or invisible in optical images, although they are located just a few arcminutes south of the (much less obscured and therefore optically much brighter) stars of the cluster Tr 16.…”

Section: Introductionmentioning

confidence: 99%

Gaia EDR3 distances of the young stellar clusters in the extended Carina Nebula complex

Göppl,

Preibisch

2022

Preprint

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Context. The Carina Nebula complex (CNC) is one of the most massive and active star-forming regions in our Galaxy and it contains several large young star clusters. The distances of the individual clusters and their physical connection were poorly known up to now, with strongly discrepant results reported in the literature. Aims. We want to determine reliable distances of the young stellar clusters in the central Carina Nebula region (in particular, Tr 14, 15, and 16) and the prominent clusters NGC 3324 and NGC 3293 in the northwestern periphery of the CNC. Methods. We analyzed the parallaxes in Gaia EDR3 for a comprehensive sample of 237 spectroscopically identified OB stars, as well as for 9562 X-ray-selected young stars throughout the complex. We also performed an astrometric analysis to identify members of the young cluster vdBH 99, which is located in the foreground of the northwestern part of the Carina Nebula. Results. We find that the distances of the investigated clusters in the CNC are equal within ≤ 2%, and yield very consistent most likely mean distance values of 2.36 +0.05 −0.05 kpc for the OB star sample and 2.34 +0.05 −0.06 kpc for the sample of X-ray-selected young stars. Conclusions. Our results show that the clusters in the CNC constitute a coherent star-forming region, in particular with regard to NGC 3324 and NGC 3293 at the northwestern periphery, which are (within ≤ 2%) at the same distance as the central Carina Nebula. For the foreground cluster vdBH 99, we find a mean distance of 441 +2 −2 pc and an age of 60 Myr. We quantified the contamination of X-ray-selected samples of Carina Nebula stars based on members of this foreground cluster.

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Detection of new O-type stars in the obscured stellar cluster Tr 16-SE in the Carina Nebula with KMOS

Cited by 9 publications

References 46 publications

The Villafranca catalog of Galactic OB groups

The Villafranca catalog of Galactic OB groups

Characterizing the X-Ray Emission of Intermediate-mass Pre-main-sequence Stars

Gaia EDR3 distances of the young stellar clusters in the extended Carina Nebula complex

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