208 research outputs found
Spectroscopic characterization of X-ray emitting young stars associated with the Sh 2-296 nebula
We studied a sample of stars associated with the Sh 2-296 nebula, part of the
reflection nebulae complex in the region of Canis Major (CMa R1). Our sample
corresponds to optical counterparts of X-ray sources detected from observations
with the XMM-Newton satellite, which revealed dozens of possible low-mass young
stars not yet known in this region.
A sample of 58 young star candidates were selected based on optical spectral
features, mainly H{\alpha} and lithium lines, observed with multi-objects
spectroscopy performed by the Gemini South telescope. Among the candidates, we
find 41 confirmed T Tauri and 15 very likely young stars. Based on the
H{\alpha} emission, the T Tauri stars were distinguished between classical
(17%) and weak-lined (83%), but no significant difference was found in the age
and mass distribution of these two classes.
The characterization of the sample was complemented by near- and mid-infrared
data, providing an estimate of ages and masses from the comparison with
pre-main-sequence evolutionary models. While half of the young stars have an
age of 1-2 Myrs or less, only a small fraction (~25%) shows evidence of IR
excess revealing the presence of circumstellar discs. This low fraction is
quite rare compared to most young star-forming regions, suggesting that some
external factor has accelerated the disc dissipation
Excess gamma-rays in the direction of the rho Ophiuchi cloud: An exotic object?
The COS-B X-ray data in the direction of the rho Oph dark cloud show an extended structure; at the same time, the region of highest intensity has a spatial distribution compatible with a localized source; 2CG353+16 which is designated Oph gamma. The possibility of an excess gamma ray flux over what is expected on the basis of the interaction of average density cosmic rays with an estimated cloud mass of 2 to 4 000 M is still open, pending an extended CO survey matching the gamma ray data. Estimates for this excess factor are in the range 2 to 4. While the cloud mass may be underestimated, it should be noted that an excess of the same order appears to be present in the nearby Oph-Sag area, well surveyed in CO with the Columbia dish. Possible reasons for a gamma ray excess, in view of two recent observational developments: an Einstein X-ray survey and a VLA radio survey, both covering the approx 2 deg diameter Oph gamma error box. Current interpretations link the gamma ray excess to the cloud gas, in which some active agent is present: stellar winds, or interaction with the North Polar Spur
Star formation history of Canis Major OB1 - II. A bimodal X-ray population revealed by XMM-Newton
The Canis Major OB1 Association has an intriguing scenario of star formation,
especially in the Canis Major R1 (CMa R1) region traditionally assigned to a
reflection nebula, but in reality an ionized region. This work is focused on
the young stellar population associated to CMa R1, for which our previous
results from ROSAT, optical and near-infrared data had revealed two stellar
groups with different ages, suggesting a possible mixing of populations
originated from distinct star-formation episodes. The X-ray data allow the
detected sources to be characterized according to hardness ratios, light curves
and spectra. Estimates of mass and age were obtained from the 2MASS catalogue,
and used to define a complete subsample of stellar counterparts, for
statistical purposes. A catalogue of 387 XMM-Newton sources is provided, 78%
being confirmed as members or probable members of the CMa R1 association.
Flares were observed for 13 sources, and the spectra of 21 bright sources could
be fitted by a thermal plasma model. Mean values of fits parameters were used
to estimate X-ray luminosities. We found a minimum value of log(L[erg/s]) =
29.43, indicating that our sample of low-mass stars (M 0.5
M), being faint X-ray emitters, is incomplete. Among the 250 objects
selected as our complete subsample (defining our best sample), 171 are found to
the East of the cloud, near Z CMa and dense molecular gas, 50% of them being
young ( 10 Myr). The opposite happens to the
West, near GU CMa, in areas lacking molecular gas: among 79 objects, 30% are
young and 50% are older. These findings confirm that a first episode of
distributed star formation occurred in the whole studied region ~10 Myr ago and
dispersed the molecular gas, while a second, localized episode (< 5 Myr) took
place in the regions where molecular gas is still present.Comment: 38 pages, 21 figures, accepted for A&
Discovery of new embedded Herbig-Haro objects in the rho Ophiuchi dark cloud
We report here the discovery of a 30"-chain of embedded Herbig-Haro (HH) objects in the rho Ophiuchi dark cloud. These HH objects were first detected during a deep K_S-band observation (completeness magnitude for point source~19) made with NTT/SOFI. We confirm their nature with follow-up observations made with H_2 v=1-0 S(1) narrow-band filter. We argue that they belong to two different jets emanating from two Class I protostars: the main component of the recently resolved subarcsecond radio binary YLW15 (also called IRS43), and IRS54. We propose also to identify the [S II] knot HH224NW1 (Gomez et al 1998) as emanating from a counterjet of YLW15. The alignment between these HH objects and the thermal jet candidate found in YLW15 by Girart et al. (2000) implies that this jet is not precessing at least on timescale ~(2-4)x1E4 yr
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