X-ray properties of the young open clusters HM1 and IC 2944/2948

Nazé, Yaël; Rauw, Grégor; Sana, H.; Corcoran, M. F.

doi:10.1051/0004-6361/201321099

Cited by 18 publications

(27 citation statements)

References 57 publications

(117 reference statements)

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“…Double symbols indicate binary stars. X symbols and red dots are, respectively, x-ray sources (Nazé et al 2013) and MSX sources (Lumsden et al 2002) correlated with our data.…”

Section: Photometrysupporting

confidence: 82%

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A deep and wide-field view at the IC 2944/2948 complex in Centaurus*

Baume

Rodríguez

Corti

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We employed the ESO MPI wide-field camera and obtained deep images in the VI C passbands in the region of the IC 2944/2948 complex (l ∼ 294. • 8; b ∼ −1. • 6), and complemented them with literature and archival data. We used this material to derive the photometric, spectroscopic and kinematic properties of the brightest (V < 16) stars in the region. The VI deep photometry on the other end, helped us to unravel the lower main sequence of a few, possibly physical, star groups in the area.Our analysis confirmed previous suggestions that the extinction toward this line of sight follows the normal law (R V = 3.1). We could recognize B-type stars spread in distance from a few hundred pc to at least 2 kpc. We found two young groups (age ∼ 3 Myr) located respectively at about 2.3 and 3.2 kpc from the Sun. They are characterized by a significant variable extinction (E B−V ranging from 0.28 to 0.45 mag), and host a significant pre-main sequence population. We computed the initial mass functions for these groups and obtained slopes Γ from -0.94 to -1.02 (e Γ = 0.3), in a scale where the classical Salpeter law is -1.35. We estimated the total mass of both main stellar groups in ∼ 1100 and ∼ 500 M ⊙ , respectively. Our kinematic analysis indicated that both groups of stars deviate from the standard rotation curve of the Milky Way, in line with literature results for this specific Galactic direction.Finally, along the same line of sight we identified a third group of early-type stars located at ∼ 8 kpc from the Sun. This group might be located in the far side of the Sagittarius-Carina spiral arm.

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“…Double symbols indicate binary stars. X symbols and red dots are, respectively, x-ray sources (Nazé et al 2013) and MSX sources (Lumsden et al 2002) correlated with our data.…”

Section: Photometrysupporting

confidence: 82%

“…• More recently, Nazé et al (2013) studied for the first time this region using XMM-Newton data and claimed for the existence of a tight cluster.…”

Section: Introductionmentioning

confidence: 99%

A deep and wide-field view at the IC 2944/2948 complex in Centaurus*

Baume

Rodríguez

Corti

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…sive binaries observed with ROSAT, Sana et al (2006) for O-type stars in NGC 6231, Nazé (2009) for the general sample of O-type stars observed with XMM-Newton, Nazé et al (2011) for the O-stars in the Carina complex, and, most recently, by Nazé et al (2013b) for the O-star population of IC 2944-8 and Havlen-Moffat 1. In our sample, the strongest over-luminosities are found for CPR2002 A26, CPR2002 A20, MT91 516, and CPR2002 A11.…”

Section: The L X /L Bol Relation Of O-stars In Cyg Ob2mentioning

confidence: 99%

X-Ray Emission From Massive Stars in Cyg Ob2

Rauw

Nazé

Wright

et al. 2015

ApJS

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We report on the analysis of the Chandra-ACIS data of O, B, and WR stars in the young association Cyg OB2. X-ray spectra of 49 O-stars, 54 B-stars, and 3 WR-stars are analyzed and for the brighter sources, the epoch dependence of the X-ray fluxes is investigated. The O-stars in Cyg OB2 follow a well-defined scaling relation between their X-ray and bolometric luminosities:This relation is in excellent agreement with the one previously derived for the Carina OB1 association. Except for the brightest O-star binaries, there is no general X-ray overluminosity due to colliding winds in O-star binaries. Roughly half of the known B-stars in the surveyed field are detected, but they fail to display a clear relationship between L X and L bol . Out of the three WR stars in Cyg OB2, probably only WR 144 is itself responsible for the observed level of X-ray emission, at a very low log 8.8 0.2The X-ray emission of the other two WR-stars (WR 145 and 146) is most probably due to their O-type companion along with a moderate contribution from a wind-wind interaction zone.

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“…This relation reflects an intimate link between X-rays and the stellar winds, as X-rays are produced behind shocks in these unstable outflows, although a full understanding of the origin of the relation is still lacking (steps in this direction have been taken by Oskinova et al 2011;Owocki et al 2013). Different log(L X /L BOL ) values have been reported in the literature for Galactic objects, but these differences are probably explained by choices made in the analysis (e.g., method for deriving L BOL ) and the data quality (Nazé et al 2011(Nazé et al , 2013.…”

Section: Detection Of Massive X-ray Emitters In N11mentioning

confidence: 99%

A DEEP CHANDRA OBSERVATION OF THE GIANT H II REGION N11. I. X-RAY SOURCES IN THE FIELD

Nazé

Wang

Chu

et al. 2014

ApJS

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A very sensitive X-ray investigation of the giant H ii region N11 in the Large Megallanic Cloud was performed using the Chandra X-ray Observatory. The 300 ks observation reveals X-ray sources with luminosities down to 10 32 erg s −1 , increasing the number of known point sources in the field by more than a factor of five. Among these detections are 13 massive stars (3 compact groups of massive stars, 9 O stars, and one early B star) with log(L X /L BOL ) ∼ −6.5 to −7, which may suggest that they are highly magnetic or colliding-wind systems. On the other hand, the stacked signal for regions corresponding to undetected O stars yields log(L X /L BOL ) ∼ −7.3, i.e., an emission level comparable to similar Galactic stars despite the lower metallicity. Other point sources coincide with 11 foreground stars, 6 late-B/A stars in N11, and many background objects. This observation also uncovers the extent and detailed spatial properties of the soft, diffuse emission regions, but the presence of some hotter plasma in their spectra suggests contamination by the unresolved stellar population.

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X-ray properties of the young open clusters HM1 and IC 2944/2948

Cited by 18 publications

References 57 publications

A deep and wide-field view at the IC 2944/2948 complex in Centaurus*

A deep and wide-field view at the IC 2944/2948 complex in Centaurus*

X-Ray Emission From Massive Stars in Cyg Ob2

A DEEP CHANDRA OBSERVATION OF THE GIANT H II REGION N11. I. X-RAY SOURCES IN THE FIELD

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