58 research outputs found
Coherent transfer of photoassociated molecules into the rovibrational ground state
We report on the direct conversion of laser-cooled 41K and 87Rb atoms into
ultracold 41K87Rb molecules in the rovibrational ground state via
photoassociation followed by stimulated Raman adiabatic passage.
High-resolution spectroscopy based on the coherent transfer revealed the
hyperfine structure of weakly bound molecules in an unexplored region. Our
results show that a rovibrationally pure sample of ultracold ground-state
molecules is achieved via the all-optical association of laser-cooled atoms,
opening possibilities to coherently manipulate a wide variety of molecules.Comment: 4 pages, 4 figure
Young Brown Dwarfs in the Core of the W3 Main Star-Forming Region
We present the results of deep and high-resolution (FWHM ~ 0".35) JHK NIR
observations with the Subaru telescope, to search for very low mass young
stellar objects (YSOs) in the W3 Main star-forming region. The NIR survey
covers an area of ~ 2.6 arcmin^2 with 10-sigma limiting magnitude exceeding 20
mag in the JHK bands. The survey is sensitive enough to provide unprecedented
details in W3 IRS 5 region and reveals a census of the stellar population down
to objects below the hydrogen-burning limit. We construct JHK color-color (CC)
and J-H/J and H-K/K color-magnitude (CM) diagrams to identify very low
luminosity YSOs and to estimate their masses. Based on these CC and CM
diagrams, we identified a rich population of embedded YSO candidates with
infrared excesses (Class I and Class II), associated with the W3 Main region. A
large number of red sources (H-K > 2) have also been detected around W3 Main.
We argue that these red stars are most probably pre-main-sequence (PMS) stars
with intrinsic color excesses. Based on the comparison between theoretical
evolutionary models of very low-mass PMS objects with the observed CM diagram,
we find there exists a substantial substellar population in the observed
region. The mass function (MF) does not show the presence of cutoff and sharp
turnover around the substellar limit, at least at the hydrogen-burning limit.
Furthermore, the MF slope indicates that the number ratio of young brown dwarfs
and hydrogen-burning stars in the W3 Main is probably higher than those in
Trapezium and IC 348. The presence of mass segregation, in the sense that
relatively massive YSOs lie near the cluster center, is seen. The estimated
dynamical evolution time indicates that the observed mass segregation in the W3
Main may be the imprint of the star formation process.Comment: 39 pages, 15 figures. Accepted for publication in the Astrophysical
Journa
Interferometric Observations of the T Tauri Stars in the MBM 12 Cloud
We have carried out a millimeter interferometric continuum survey toward 7
YSOs in the MBM 12 cloud. Thermal emissions associated with 2 YSOs were
detected above the 3- level at 2.1 mm, and one also showed a 1.3 mm
thermal emission. Another object was marginally detected at 2.1 mm. Spectral
energy distributions of the YSOs are well fitted by a simple power-law disk
model. Masses of the circumstellar disks are estimated to be an order of 0.05
M_{\sun}. The circumstellar disks in the MBM 12 cloud have properties in
common with the disks in nearby star-forming regions, in terms of disk
parameters such as a disk mass, as well as an infrared excess.Comment: 9 pages, 3 figures, accepted by ApJ Letter
The stellar content of the young open cluster Trumpler 37
With an apparent cluster diameter of 1.5{\deg} and an age of ~4 Myr, Trumpler
37 is an ideal target for photometric monitoring of young stars as well as for
the search of planetary transits, eclipsing binaries and other sources of
variability. The YETI consortium has monitored Trumpler 37 throughout 2010 and
2011 to obtain a comprehensive view of variable phenomena in this region. In
this first paper we present the cluster properties and membership determination
as derived from an extensive investigation of the literature. We also compared
the coordinate list to some YETI images. For 1872 stars we found literature
data. Among them 774 have high probability of being member and 125 a medium
probability. Based on infrared data we re-calculate a cluster extinction of
0.9-1.2 mag. We can confirm the age and distance to be 3-5 Myr and ~870 pc.
Stellar masses are determined from theoretical models and the mass function is
fitted with a power-law index of alpha=1.90 (0.1-0.4 M_sun) and alpha=1.12
(1-10 M_sun).Comment: 9 pages, 10 figures, 2 long tables, accepte
The ratio of N(C18O) and Av in Chamaeleon I and III-B using 2MASS and SEST
We investigate the relationship between the C18O column density and the
visual extinction in Chamaeleon I and in a part of the Chamaeleon III molecular
cloud. The C18O column densities, N(C18O), are calculated from J=1-0 rotational
line data observed with the SEST telescope. The visual extinctions, Av, are
derived using JHK photometry from the 2MASS survey and the NICER color excess
technique. In contrast with the previous results of Hayakawa et al. (2001), we
find that the average N(C18O) / Av ratios are similar in Cha I and Cha III, and
lie close to values derived for other clouds, i.e. N(C18O) ~ 2 x 10^14 cm^-2
(Av - 2). We find, however, clear deviations from this average relationship
towards individual clumps. Larger than average N(C18O) / Av ratios can be found
in clumps associated with the active star forming region in the northern part
of Ch a I. On the other hand, some regions in the relatively quiescent southern
part of Cha I show smaller than average N(C18O) / Av ratios and also very
shallow proportionality between N(C18O) and Av. The shallow proportionality
suggests that C18O is heavily depleted in these regions. As the degree of
depletion is proportional to the gas density, these regions probably contain
very dense, cold cores, which do not stand out in CO mappings. A comparison
with the dust temperature map derived from the ISO data shows that the most
prominent of the potentially depleted cores indeed coincides with a dust
temperature minimum. It seems therefore feasible to use N(C18O) and Av data
together for identifying old, dense cores in large scale mappings.Comment: 15 pages, 8 figures. Accepted for publication in A&A. Replaced with a
version with corrected illustration
Multi-wavelength study of a young open cluster NGC 7419
Using UBVRI Halpha CCD photometric observations and the archival NIR and
X-ray data, we have carried out a multi-wavelength study of a young star
cluster NGC 7419. An age of 22.5+/-3.0 Myr and a distance of 3230^{+330}_{-430}
pc are derived for the cluster with a higher value of color excess ratio
E(U-B)/E(B-V) than the normal one. There is an evidence for mass segregation in
this dynamically relaxed cluster with mass function slope is in agreement with
the Salpeter value. NIR and Halpha excess support the existence of a young (< 2
Myr) stellar population of Herbig Ae/Be stars (> 3.0 M_sun) indicating a second
episode of star formation in the cluster region. Using XMM-Newton observations,
we found several X-ray sources in the cluster region but none of the Herbig
Ae/Be stars is detected in X-rays. We compare the distribution of upper limits
for Herbig Ae/Be stars with the X-ray distribution functions of the T-Tauri and
the Herbig Ae/Be stars from previous studies, and found that the X-ray emission
level of these Herbig Ae/Be stars is not more than L_X ~5.2 x 10^{30} erg/s,
which is not significantly higher than for the T-Tauri stars. Therefore, X-ray
emission from Herbig Ae/Be stars could be the result of either unresolved
companion stars or a process similar to T-Tauri stars. We report an extended
X-ray emission from the cluster region NGC 7419, with a total L_X estimate of ~
1.8 x 10^31 erg/s/arcmin^2. Investigation of dust and CO map of 1 degree region
around the cluster indicates the presence of a foreground dust cloud which is
most likely associated with star forming region Sh2-154. This cloud harbors
uniformly distributed pre main sequence stars (0.1-2.0M_sun) and the star
formation in this cloud depend mostly upon the primordial fragmentation.Comment: 23 pages, 23 figures, 13 tables; Accepted for publication in MNRA
A Spitzer IRS Survey of NGC 1333: Insights into disk evolution from a very young cluster
We report on the {\lambda} = 5-36{\mu}m Spitzer Infrared Spectrograph spectra
of 79 young stellar objects in the very young nearby cluster NGC 1333. NGC
1333's youth enables the study of early protoplanetary disk properties, such as
the degree of settling as well as the formation of gaps and clearings. We
construct spectral energy distributions (SEDs) using our IRS data as well as
published photometry and classify our sample into SED classes. Using
"extinction-free" spectral indices, we determine whether the disk, envelope, or
photosphere dominates the spectrum. We analyze the dereddened spectra of
objects which show disk dominated emission using spectral indices and
properties of silicate features in order to study the vertical and radial
structure of protoplanetary disks in NGC 1333. At least nine objects in our
sample of NGC 1333 show signs of large (several AU) radial gaps or clearings in
their inner disk. Disks with radial gaps in NGC 1333 show more-nearly pristine
silicate dust than their radially continuous counterparts. We compare
properties of disks in NGC 1333 to those in three other well studied regions,
Taurus-Auriga, Ophiuchus and Chamaeleon I, and find no difference in their
degree of sedimentation and dust processing.Comment: 67 pages, 20 figures, accepted to The Astrophysical Journal
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