X-ray survey of the North-America and Pelican star-forming complex (NGC 7000/IC 5070)

Damiani, F.; Pillitteri, I.; Prisinzano, L.

doi:10.1051/0004-6361/201629402

Cited by 17 publications

(27 citation statements)

References 50 publications

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“…4e shows an optical-NIR color-color diagram, useful to select Class II PMS stars with disk-related NIR excesses. As in Paper I (and already argued in Damiani et al 2006a, 2017b, or Guarcello et al 2007), this mixed optical-NIR diagram selects more objects than the (J − H, H − K) diagram (not shown here), being sensitive even to weaker excesses in spite of requiring data at more bands. We find 2173 NIR-excess stars selected from Fig.…”

Section: Hα Emission Nir and Uv Excessessupporting

confidence: 83%

Wide-area photometric and astrometric (Gaia DR2) study of the young cluster NGC 6530

Damiani

Prisinzano

Micela

et al. 2019

A&A

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Context. NGC 6530 is a young cluster, with a complex morphology and star-formation history. We present a statistical study of its global properties, using a new, large list of candidate members down to masses of 0.2 − 0.4M and Gaia DR2 astrometry. Aims. We consider a larger sky region compared to previous studies, to investigate the entire cluster until its periphery, including any diffuse population all around the main cluster. We study the distribution of extinction and age across the different regions, and obtain constraints on the star-formation history. We also study the dynamics of cluster members. Methods. Cluster membership is determined on the basis of literature X-ray data, Hα emission, near-IR and UV excesses from the VPHAS+ and UKIDSS photometric surveys and published near-IR catalogs, and Gaia DR2 astrometry; moreover, we use a method for photometric selection of M-type pre-main-sequence cluster members, which we recently developed and used for other star-formation regions. The list of candidates includes nearly 3700 stars, of which we estimate approximately 2700 genuine NGC 6530 members. Results. Using Gaia parallaxes, the cluster distance is found to be 1325 pc, with errors of 0.5% (statistical) and 8.5% (systematic), in agreement with previous determinations. The cluster morphology and boundaries are established with great confidence, from the agreement between the subsamples of members selected using different criteria. There is no diffuse population of members around the cluster, but there are minor condensations of true members in addition to the two main groups in the cluster core and in the Hourglass nebula. Two such subgroups are spatially associated with the stars 7 Sgr (F2II-III) and HD 164536 (O7.5V). There is a definite pattern of sequential star formation across the cluster, within an age range from less than 0.5 Myr to ∼ 5 Myr. Extinction is spatially non-uniform, with part of the population still embedded or obscured by thick dust. The precise Gaia proper motion data indicate that the NGC 6530 parent cloud collided with the Galactic plane around 4 Myr ago, and we suggest that event as the trigger of the bulk of star formation in NGC 6530. The internal cluster dynamics is also partially resolved by the Gaia data, indicating expansion of the main cluster population with respect to its center.

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Section: Hα Emission Nir and Uv Excessessupporting

confidence: 83%

Wide-area photometric and astrometric (Gaia DR2) study of the young cluster NGC 6530

Damiani

Prisinzano

Micela

et al. 2019

A&A

Self Cite

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“…The large number of likely M-type PMS stars selected in this work are consistent with results recently discussed in Damiani (2018) and are related to the higher intrinsic brightness of PMS M-type stars, with respect to MS M-type stars. This implies that at a given mass, a 1 Myr old M star can be detected at a distance much larger than a MS M star (Damiani, 2018).…”

Section: Spatial Distribution Analysissupporting

confidence: 91%

“…These values have been estimated at the peak of the magnitude distribution. As described in Damiani (2018), the minimum mass detected at a given distance strongly depends on the age and the absorption A V (see Fig. 5 of Damiani, 2018 the mass ranges were derived from the 4 and 5 Myr isochrones for i-K>2.2, that is the color limit used for the selection of M-type stars (see Fig.…”

Section: Discussionmentioning

confidence: 99%

“…On the contrary, objects with excesses in the H or K bands can be very well discriminated from reddened objects if the diagram involves an optical color, dominated by photospheric emission even in Class II stars. For example, as discussed in Damiani et al (2017), in the r-i vs. J-H and/or r-i vs. H-K diagrams, objects with excesses in the H-K or J-H colors can be confidently found on the red side of the main locus of normal reddened stars.…”

Section: Candidate Disk-bearing Young Stars From Nir Excessesmentioning

confidence: 98%

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Low-mass star formation and subclustering in the H II regions RCW 32, 33, and 27 of the Vela Molecular Ridge

Prisinzano

Damiani

Guarcello

et al. 2018

A&A

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Context. Most stars born in clusters and recent results suggest that star formation (SF) preferentially occurs in subclusters. Studying the morphology and SF history of young clusters is crucial to understanding early cluster formation processes. Aims. We aim to identify the embedded population of young stellar objects (YSOs) down to the low mass stars in the M-type regime, in the three H II regions RCW 33, RCW 32 and RCW 27 located in the northwestern region of the Vela Molecular Ridge. Our aim is to characterise their properties, such as morphology and extent of the clusters in the three H II regions, derive stellar ages and the connection of the SF history with the environment. Methods. Through public photometric surveys such as Gaia, VPHAS, 2MASS and Spitzer/GLIMPSE, we identify YSOs with classical techniques aimed at detecting IR, Hα and UV excesses, as signature of circumstellar disks and accretion. In addition, we implement a method to distinguish main sequence (MS) stars and giants in the M-type regime, by comparing the reddening derived in several optical/IR color-color diagrams, assuming suitable theoretical models. Since this diagnostic is sensitive to stellar gravity, the procedure allows us to identify also pre-main sequence (PMS) stars. Results. Using the classical membership criteria, we find a large population of YSOs showing signatures of circumstellar disks with or without accretion. In addition, with the new technique of M-type star selection, we find a rich population of young M-type stars with a spatial distribution strongly correlated to the more massive population. We find evidence of three young clusters, with different morphology, for which we estimate the individual distances by using TGAS Gaia data of the brighter subsample. In addition, we identify field stars falling in the same region, by securely classifying them as giants and foreground MS stars. Conclusions. We identify the embedded population of YSOs, down to about 0.1 M , associated with the three H II regions RCW 33, RCW 32 and RCW 27 and the three clusters Vela T2, Cr 197 and Vela T1, respectively. All the three clusters are located at a similar distance but show very different morphologies. Our results suggest a decreasing SF rate in Vela T2 and triggered SF in Cr 197 and Vela T1.

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“…NGC 7000: V1057 Cyg and HBC 722 are both probable members of NGC 7000. We find a median parallax of 1.21 mas for member candidates from the catalog of Damiani et al (2017), corresponding to 795 pc.…”

Section: A1 Detected Sourcesmentioning

confidence: 80%

A Comparison of the X-Ray Properties of FU Ori-type Stars to Generic Young Stellar Objects

Kuhn

Hillenbrand

2019

ApJ

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Like other young stellar objects (YSOs), FU Ori-type stars have been detected as strong X-ray emitters. However, little is known about how the outbursts of these stars affect their X-ray properties. We assemble available X-ray data from XMM Newton and Chandra observations of 16 FU Ori stars, including a new XMM Newton observation of Gaia 17bpi during its optical rise phase. Of these stars, six were detected at least once, while 10 were non-detections, for which we calculate upper limits on intrinsic X-ray luminosity (L X ) as a function of plasma temperature (kT ) and column density (N H ). The detected FU Ori stars tend to be more X-ray luminous than typical for non-outbursting YSOs, based on comparison to a sample of low-mass stars in the Orion Nebula Cluster. FU Ori stars with high L X have been observed both at the onset of their outbursts and decades later. We use the Kaplan-Meier estimator to investigate whether the higher X-ray luminosities for FU Ori stars is characteristic or a result of selection effects, and we find the difference to be statistically significant (p < 0.01) even when non-detections are taken into account. The additional X-ray luminosity of FU Ori stars relative to non-outbursting YSOs cannot be explained by accretion shocks, given the high observed plasma temperatures. This suggests that, for many FU Ori stars, either 1) the outburst leads to a restructuring of the magnetosphere in a way that enhances X-ray emission, or 2) FU Ori outbursts are more likely to occur among YSOs with the highest quiescent X-ray luminosity.

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X-ray survey of the North-America and Pelican star-forming complex (NGC 7000/IC 5070)

Cited by 17 publications

References 50 publications

Wide-area photometric and astrometric (Gaia DR2) study of the young cluster NGC 6530

Wide-area photometric and astrometric (Gaia DR2) study of the young cluster NGC 6530

Low-mass star formation and subclustering in the H II regions RCW 32, 33, and 27 of the Vela Molecular Ridge

A Comparison of the X-Ray Properties of FU Ori-type Stars to Generic Young Stellar Objects

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X-ray survey of the North-America and Pelican star-forming complex (NGC 7000/IC 5070)

Cited by 17 publications

References 50 publications

Wide-area photometric and astrometric (Gaia DR2) study of the young cluster NGC 6530

Wide-area photometric and astrometric (Gaia DR2) study of the young cluster NGC 6530

Low-mass star formation and subclustering in the H II regions RCW 32, 33, and 27 of the Vela Molecular Ridge

A Comparison of the X-Ray Properties of FU Ori-type Stars to Generic Young Stellar Objects

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Low-mass star formation and subclustering in the H II regions RCW 32, 33, and 27 of the Vela Molecular Ridge