An $\vec{XMM}$-$\vec{Newton}$ observation of the Lagoon Nebula and the very young open cluster NGC 6530

Rauw, Grégor; Nazé, Yaël; Gosset, Éric; Stevens, I. R.; Blomme, R.; Corcoran, M. F.; Pittard, J. M.; Runacres, Mark

doi:10.1051/0004-6361:20021230

Cited by 42 publications

(61 citation statements)

References 41 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For many years, this star was presumed to be a single source. The situation only changed when its X-ray properties as well as episodic variations of some optical line profiles over long timescales were interpreted as signatures of a long-period (eight to nine years) eccentric double-lined spectroscopic binary (SB2) system (Rauw et al 2002a, hereafter Paper I; Rauw et al 2005). This scenario was confirmed when we obtained a first orbital solution of 9 Sgr (Rauw et al 2012, hereafter Paper II), and when phase-locked variations of the radio flux at 2 cm were reported by Blomme & Volpi (2014, hereafter Paper III).…”

Section: Postdoctoral Researcher Frs-fnrs (Belgium) Senior Research mentioning

confidence: 99%

Testing the theory of colliding winds: the periastron passage of 9 Sagittarii

Rauw

Blomme

Nazé

et al. 2016

A&A

Self Cite

View full text Add to dashboard Cite

Context. The long-period, highly eccentric O-star binary 9 Sgr, known for its non-thermal radio emission and its relatively bright X-ray emission, went through its periastron in 2013. Aims. Such an event can be used to observationally test the predictions of the theory of colliding stellar winds over a broad range of wavelengths. Methods. We conducted a multi-wavelength monitoring campaign of 9 Sgr around the 2013 periastron. In this paper, we focus on X-ray observations and optical spectroscopy. Results. The optical spectra allow us to revisit the orbital solution of 9 Sgr and to refine its orbital period to 9.1 years. The X-ray flux is maximum at periastron over all energy bands, but with clear differences as a function of energy. The largest variations are observed at energies above 2 keV, whilst the spectrum in the soft band (0.5−1.0 keV) remains mostly unchanged, indicating that it arises far from the collision region, in the inner winds of the individual components. The level of the hard emission at periastron clearly deviates from the 1/r relation expected for an adiabatic wind-interaction zone, whilst this relation seems to hold at the other phases that are covered by our observations. The spectra taken at phase 0.946 reveal a clear Fe xxv line at 6.7 keV, but no such line is detected at periastron (φ = 0.000), although a simple model predicts a strong line that should be easily visible in the data. Conclusions. The peculiarities of the X-ray spectrum of 9 Sgr could reflect the effect of radiative inhibition as well as a phasedependent efficiency of particle acceleration on the shock properties.

show abstract

Section: Postdoctoral Researcher Frs-fnrs (Belgium) Senior Research mentioning

confidence: 99%

Testing the theory of colliding winds: the periastron passage of 9 Sagittarii

Rauw

Blomme

Nazé

et al. 2016

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…In particular, following up on pioneering ROSAT observations, intermediate to distant clouds have been covered by Chandra: the Orion nebula (Garmire et al 2000;Feigelson et al 2002Feigelson et al , 2003Flaccomio et al 2003), part of the Rosette nebula and molecular cloud, together with M17 (Townsley et al 2003;Wang et al 2008Wang et al , 2009); Mon R2 (Kohno et al 2002); RCW38 (Wolk et al 2002); M16 (Linsky et al 2007), and by XMMNewton: M8 (Rauw et al 2002); Carina (Albacete Colombo et al 2003); Vela OB2 (Jeffries et al 2009); Orion (López-Santiago & Caballero 2008); and others. Up to thousands of point X-ray sources per cloud are detected, almost all identified with young stars, down to the brown dwarf regime.…”

Section: Search For Young Stars Based On X-ray Datamentioning

confidence: 99%

Star formation history of Canis Major R1

Gregorio-Hetem¹,

Montmerle

Rodrigues

et al. 2009

A&A

View full text Add to dashboard Cite

Aims. The CMa R1 star-forming region contains several compact clusters as well as many young early-B stars. It is associated with a well-known bright rimmed nebula, the nature of which is unclear (fossil HII region or supernova remnant). To help elucidate the nature of the nebula, our goal was to reconstruct the star-formation history of the CMa R1 region, including the previously unknown older, fainter low-mass stellar population, using X-rays. Methods. We analyzed images obtained with the ROSAT satellite, covering ∼5 sq. deg. Complementary VRI photometry was performed with the Gemini South telescope. Colour-magnitude and colour-colour diagrams were used in conjunction with pre-main sequence evolutionary tracks to derive the masses and ages of the X-ray sources.Results. The ROSAT images show two distinct clusters. One is associated with the known optical clusters near Z CMa, to which ∼40 members are added. The other, which we name the "GU CMa" cluster, is new, and contains ∼60 members. The ROSAT sources are young stars with masses down to M ∼ 0.5 M , and ages up to 10 Myr. The mass functions of the two clusters are similar, but the GU CMa cluster is older than the cluster around Z CMa by at least a few Myr. Also, the GU CMa cluster is away from any molecular cloud, implying that star formation must have ceased; on the contrary (as already known), star formation is very active in the Z CMa region.

show abstract

“…Loktin et al (1997) 1800 11.25 Sung et al (2000) 560-711 8.75-9.26 Loktin & Beshenov (2001) low mass stars are expected to be still in the pre-main sequence phase, as already found in Sung et al (2000) from photometric data down to the limiting magnitude V ∼ 17. 119 X-ray point sources in the Lagoon Nebula region have been recently detected by Rauw et al (2002) in a 20 ks XMM-Newton observation; they found that most of the X-ray sources are associated with pre-main sequence stars of low and intermediate mass. However, a larger list of point sources in the same region, with a much better spatial resolution, has recently been obtained by Damiani et al (2004), using Chandra ACIS-I X-ray data.…”

Section: Introductionmentioning

confidence: 99%

The star formation region NGC 6530: Distance, ages and initial mass function

Prisinzano

Damiani

Micela

et al. 2005

A&A

158

View full text Add to dashboard Cite

Abstract. We present astrometry and BV I photometry, down to V 22, of the very young open cluster NGC 6530, obtained from observations taken with the Wide Field Imager camera at the MPG/ESO 2.2 m Telescope. Both the V vs. B − V and the V vs. V − I color−magnitude diagrams (CMD) show that the upper main sequence is dominated by very bright cluster stars, while, because of the high obscuration of the giant molecular cloud surrounding the cluster, the blue envelopes of the diagrams at V 14 are limited to the main sequence stars at the distance of NGC 6530. This particular structure of the NGC 6530 CMD allows us to conclude that its distance is about d 1250 pc, significantly lower than the previous determination of d = 1800 pc. We have positionally matched our optical catalog with the list of X-ray sources found in a Chandra-ACIS observation, finding a total of 828 common stars, 90% of which are pre-main sequence stars in NGC 6530. Using evolutionary tracks of Siess et al. (2000), mass and age values are inferred for these stars. The median age of the cluster is about 2.3 Myr; in the mass range (0.6−4.0) M , the Initial Mass Function (IMF) shows a power law index x = 1.22 ± 0.17, consistent with both the Salpeter index (1.35), and with the index derived for other young clusters; towards smaller masses the IMF shows a peak and then it starts to decrease.

show abstract

An $\vec{XMM}$-$\vec{Newton}$ observation of the Lagoon Nebula and the very young open cluster NGC 6530

Cited by 42 publications

References 41 publications

Testing the theory of colliding winds: the periastron passage of 9 Sagittarii

Testing the theory of colliding winds: the periastron passage of 9 Sagittarii

Star formation history of Canis Major R1

The star formation region NGC 6530: Distance, ages and initial mass function

Contact Info

Product

Resources

About