81 research outputs found
Hubble Space Telescope NICMOS Imaging of W3 IRS 5: A Trapezium in the Making?
We present Hubble Space Telescope NICMOS imaging of W3 IRS 5, a binary
high-mass protostar. In addition to the two protostars, NICMOS images taken in
the F222M and F160W filters show three new 2.22 micron sources with very red
colors; these sources fall within a region 5600 AU in diameter, and are
coincident with a 100 solar mass dense molecular clump. Two additional point
sources are found within 0.4'' (800 AU) of one of the high-mass protostars;
these may be stellar companions or unresolved emission knots from an outflow.
We propose that these sources constitute a nascent Trapezium system in the
center of the W3 IRS 5 cluster containing as many as five proto OB stars. This
would be the first identification of a Trapezium still deeply embedded in its
natal gas.Comment: accepted to ApJ letter
High-Resolution Continuum Imaging at 1.3 and 0.7 cm of the W3 IRS 5 Region
High-resolution images of the hypercompact HII regions (HCHII) in W3 IRS 5
taken with the Very Large Array (VLA) at 1.3 and 0.7 cm are presented. Four
HCHII regions were detected with sufficient signal-to-noise ratios to allow the
determination of relevant parameters such as source position, size and flux
density. The sources are slightly extended in our ~0.2 arcsecond beams; the
deconvolved radii are less than 240 AU. A comparison of our data with VLA
images taken at epoch 1989.1 shows proper motions for sources IRS 5a and IRS
5f. Between 1989.1 and 2002.5, we find a proper motion of 210 mas at a position
angle of 12 deg for IRS 5f and a proper motion of 190 mas at a position angle
of 50 deg for IRS 5a. At the assumed distance to W3 IRS 5, 1.83 +/- 0.14 kpc,
these offsets translate to proper motions of ~135 km/s and ~122 km/s$
respectively. These sources are either shock ionized gas in an outflow or
ionized gas ejected from high mass stars. We find no change in the positions of
IRS 5d1/d2 and IRS 5b; and we show through a comparison with archival NICMOS
2.2 micron images that these two radio sources coincide with the infrared
double constituting W3 IRS 5. These sources contain B or perhaps O stars. The
flux densities of the four sources have changed compared to the epoch 1989.1
results. In our epoch 2002.5 data, none of the spectral indicies obtained from
flux densities at 1.3 and 0.7 cm are consistent with optically thin free-free
emission; IRS 5d1/d2 shows the largest increase in flux density from 1.3 cm to
0.7 cm. This may be an indication of free-free optical depth within an ionized
wind, a photoevaporating disk, or an accretion flow. It is less likely that
this increase is caused by dust emission at 0.7 cm.Comment: 13 pages, 3 figures To be published in The Astrophysical Journa
The Diverse Stellar Populations of the W3 Star Forming Complex
An 800 sq-arcmin mosaic image of the W3 star forming complex obtained with
the Chandra X-ray Observatory gives a valuable new view of the spatial
structure of its young stellar populations. The Chandra image reveals about
1300 faint X-ray sources, most of which are PMS stars in the cloud. Some, but
not all, of the high-mass stars producing hypercompact and ultracompact H II
(UCHII) regions are also seen, as reported in a previous study.
The Chandra images reveal three dramatically different embedded stellar
populations. The W3 Main cluster extends over 7 pc with about 900 X-ray stars
in a nearly-spherical distribution centered on the well-studied UCHII regions
and high-mass protostars. The cluster surrounding the prototypical UCHII region
W3(OH) shows a much smaller (<0.6 pc), asymmetrical, and clumpy distribution of
about 50 PMS stars. The massive star ionizing the W3 North H II region is
completely isolated without any accompanying PMS stars. In W3 Main, the
inferred ages of the widely distributed PMS stars are significantly older than
the inferred ages of the central OB stars illuminating the UCHIIs. We suggest
that different formation mechanisms are necessary to explain the diversity of
the W3 stellar populations: cluster-wide gravitational collapse with delayed OB
star formation in W3 Main, collect-and-collapse triggering by shock fronts in
W3(OH), and a runaway O star or isolated massive star formation in W3 North.Comment: To appear in the Astrophysical Journal. 21 pages, 5 figures. A
version with high-quality figures is available at
http://www.astro.psu.edu/users/edf/W3_Chandra.pd
Molecular Line Emission from Massive Protostellar Disks: Predictions for ALMA and the EVLA
We compute the molecular line emission of massive protostellar disks by
solving the equation of radiative transfer through the cores and disks produced
by the recent radiation-hydrodynamic simulations of Krumholz, Klein, & McKee.
We find that in several representative lines the disks show brightness
temperatures of hundreds of Kelvin over velocity channels ~10 km s^-1 wide,
extending over regions hundreds of AU in size. We process the computed
intensities to model the performance of next-generation radio and submillimeter
telescopes. Our calculations show that observations using facilities such as
the EVLA and ALMA should be able to detect massive protostellar disks and
measure their rotation curves, at least in the nearest massive star-forming
regions. They should also detect significant sub-structure and non-axisymmetry
in the disks, and in some cases may be able to detect star-disk velocity
offsets of a few km s^-1, both of which are the result of strong gravitational
instability in massive disks. We use our simulations to explore the strengths
and weaknesses of different observational techniques, and we also discuss how
observations of massive protostellar disks may be used to distinguish between
alternative models of massive star formation.Comment: 15 pages, 9 figures, emulateapj format, accepted for publication in
ApJ. Resolution of figures severely degraded to fit within size limits.
Download the full paper from
http://www.astro.princeton.edu/~krumholz/recent.htm
Signatures of inflow motion in cores of massive star formation: Potential collapse candidates
Using the IRAM 30 m telescope, a mapping survey in optically thick and thin
lines was performed towards 46 high mass star-forming regions. The sample
includes UC H{\sc ii} precursors and UC H{\sc ii} regions. Seventeen sources
are found to show "blue profiles", the expected signature of collapsing cores.
The excess of sources with blue over red profiles ([ -- ]/) is 29% in the HCO =1--0 line, with a probability
of 0.6% that this is caused by random fluctuations. UC H{\sc ii} regions show a
higher excess (58%) than UC H{\sc ii} precursors (17%), indicating that
material is still accreted after the onset of the UC H{\sc ii} phase. Similar
differences in the excess of blue profiles as a function of evolutionary state
are not observed in low mass star-forming regions. Thus, if confirmed for high
mass star-forming sites, this would point at a fundamental difference between
low- and high-mass star formation. Possible explanations are inadequate
thermalization, stronger influence of outflows in massive early cores, larger
gas reserves around massive stellar objects or different trigger mechanisms
between low- and high- mass star formation
The Early Evolution of Massive Stars: Radio Recombination Line Spectra
Velocity shifts and differential broadening of radio recombination lines are
used to estimate the densities and velocities of the ionized gas in several
hypercompact and ultracompact HII regions. These small HII regions are thought
to be at their earliest evolutionary phase and associated with the youngest
massive stars. The observations suggest that these HII regions are
characterized by high densities, supersonic flows and steep density gradients,
consistent with accretion and outflows that would be associated with the
formation of massive stars.Comment: ApJ in pres
Gaussian Spectral Line Profiles of Astrophysical Masers
Calculations are performed to demonstrate the deviations from Gaussian that
occur in the spectral line profiles of a linear maser as a result of the
amplification process. Near-Gaussian profiles are presented for bright,
interstellar 22 GHz water masers obtained from high resolution Very Long
Baseline Array (VLBA) observations of W3 IRS 5. For the profiles to be so close
to Gaussian, the calculations indicate that these masers must originate in
quite hot gas with temperatures greater than 1200 K -- a conclusion that is
supportive of C-type shocks as the origin of these masers. In addition, the
degree of saturation of these masers must be less than approximately one-third,
from which it follows that the beaming angles are less than about 10^{-4} ster
and the actual luminosities are modest. If spectral profiles that are as close
to Gaussian as the profiles presented in this initial investigation are found
to occur widely, they can be valuable diagnostics for the environments of
astrophysical masers.Comment: 4 pages with 3 figures embedded in paper; uses AASTEX with
emulateapj5.sty; accepted for publication in ApJ (Letters
Hierarchical Triggering of Star Formation by Superbubbles in W3/W4
It is generally believed that expanding superbubbles and mechanical feedback
from massive stars trigger star formation, because there are numerous examples
of superbubbles showing secondary star formation at their edges. However, while
these systems show an age sequence, they do not provide strong evidence of a
causal relationship. The W3/W4 Galactic star-forming complex suggests a
three-generation hierarchy: the supergiant shell structures correspond to the
oldest generation; these triggered the formation of IC 1795 in W3, the
progenitor of a molecular superbubble; which in turn triggered the current
star-forming episodes in the embedded regions W3-North, W3-Main, and W3-OH. We
present UBV photometry and spectroscopic classifications for IC 1795, which
show an age of 3 - 5 Myr. This age is intermediate between the reported 6 - 20
Myr age of the supergiant shell system, and the extremely young ages (10^4 -
10^5 yr) for the embedded knots of ultracompact HII regions, W3-North, W3-Main,
and W3-OH. Thus, an age sequence is indeed confirmed for the entire W3/W4
hierarchical system. This therefore provides some of the first convincing
evidence that superbubble action and mechanical feedback are indeed a
triggering mechanism for star formation.Comment: 10 pages, 6 figures; accepted to the Astronomical Journal. Figure 2
included in this submission as JPE
Embedded Stellar Clusters in the W3/W4/W5 Molecular Cloud Complex
We analyze the embedded stellar content in the vicinity of the W3/W4/W5 HII
regions using the FCRAO Outer Galaxy 12CO(J=1-0) Survey, the IRAS Point Source
Catalog, published radio continuum surveys, and new near-infrared and molecular
line observations. Thirty-four IRAS Point Sources are identified that have
far-infrared colors characteristic of embedded star forming regions, and we
have obtained K' mosaics and 13CO(J=1-0) maps for 32 of them. Ten of the IRAS
sources are associated with an OB star and 19 with a stellar cluster, although
three OB stars are not identified with a cluster. Half of the embedded stellar
population identified in the K' images is found in just the 5 richest clusters,
and 61% is contained in IRAS sources associated with an embedded OB star. Thus
rich clusters around OB stars contribute substantially to the stellar
population currently forming in the W3/W4/W5 region. Approximately 39% of the
cluster population is embedded in small clouds with an average mass of ~130 Mo
that are located as far as 100 pc from the W3/W4/W5 cloud complex. We speculate
that these small clouds are fragments of a cloud complex dispersed by previous
episodes of massive star formation. Finally, we find that 4 of the 5 known
embedded massive star forming sites in the W3 molecular cloud are found along
the interface with the W4 HII region despite the fact that most of the
molecular mass is contained in the interior regions of the cloud. These
observations are consistent with the classical notion that the W4 HII region
has triggered massive star formation along the eastern edge of the W3 molecular
cloud.Comment: to appear in ApJS, see http://astro.caltech.edu/~jmc/papers/w
- …