287 research outputs found
Radon Emanation Techniques and Measurements for LZ
Radon emanation was projected to account for % of the electron recoil
background in the WIMP region of interest for the LUX-ZEPLIN (LZ) experiment.
To mitigate the amount of radon inside the detector volume, materials with
inherently low radioactivity content were selected for LZ construction through
an extensive screening campaign. The SD Mines radon emanation system was one of
four emanation facilities utilized to screen materials during construction of
LZ. SD Mines also employed a portable radon collection system for equipment too
large or delicate to move to a radon emanation facility. This portable system
was used to assay the Inner Cryostat Vessel in-situ at various stages of
detector construction, resulting in the inference that the titanium cryostat is
the source of significant radon emanation. Assays of a Th source
confirmed that its Rn emanation is low enough for it to be used, and
that 14% of the Rn emanates from the source at room temperature.Comment: 6 pages, 4 figures, submitted to LRT 2022 Conference Proceeding
Dust emission from the Perseus molecular cloud
Using far-infrared emission maps taken by IRAS and Spitzer and a near-infrared extinction map derived from 2MASS data, we have made dust temperature and column density maps of the Perseus molecular cloud. We show that the emission from transiently heated very small grains (VSGs) and the big grain dust emissivity vary as a function of extinction and dust temperature, with higher dust emissivities for colder grains. This variable emissivity cannot be explained by temperature gradients along the line of sight or by noise in the emission maps, but it is consistent with grain growth in the higher density and lower temperature regions. By accounting for the variations in the dust emissivity and VSG emission, we are able to map the temperature and column density of a nearby molecular cloud with better accuracy than has previously been possible
TMC-1C: an accreting starless core
We have mapped the starless core TMC-1C in a variety of molecular lines with
the IRAM 30m telescope. High density tracers show clear signs of
self-absorption and sub-sonic infall asymmetries are present in N2H+ (1-0) and
DCO+ (2-1) lines. The inward velocity profile in N2H+ (1-0) is extended over a
region of about 7,000 AU in radius around the dust continuum peak, which is the
most extended ``infalling'' region observed in a starless core with this
tracer. The kinetic temperature (~12 K) measured from C17O and C18O suggests
that their emission comes from a shell outside the colder interior traced by
the mm continuum dust. The C18O (2-1) excitation temperature drops from 12 K to
~10 K away from the center. This is consistent with a volume density drop of
the gas traced by the C18O lines, from ~4x10^4 cm^-3 towards the dust peak to
~6x10^3 cm^-3 at a projected distance from the dust peak of 80" (or 11,000 AU).
The column density implied by the gas and dust show similar N2H+ and CO
depletion factors (f_D < 6). This can be explained with a simple scenario in
which: (i) the TMC-1C core is embedded in a relatively dense environment (H2
~10^4 cm^-3), where CO is mostly in the gas phase and the N2H+ abundance had
time to reach equilibrium values; (ii) the surrounding material (rich in CO and
N2H+) is accreting onto the dense core nucleus; (iii) TMC-1C is older than
3x10^5 yr, to account for the observed abundance of N2H+ across the core
(~10^-10 w.r.t. H2); and (iv) the core nucleus is either much younger (~10^4
yr) or ``undepleted'' material from the surrounding envelope has fallen towards
it in the past 10,000 yr.Comment: 29 pages, including 5 tables and 15 figure
An ALMA Search for Substructure, Fragmentation, and Hidden Protostars in Starless Cores in Chamaeleon I
We present an Atacama Large Millimeter/submillimeter Array (ALMA) 106 GHz
(Band 3) continuum survey of the complete population of dense cores in the
Chamaeleon I molecular cloud. We detect a total of 24 continuum sources in 19
different target fields. All previously known Class 0 and Class I protostars in
Chamaeleon I are detected, whereas all of the 56 starless cores in our sample
are undetected. We show that the Spitzer+Herschel census of protostars in
Chamaeleon I is complete, with the rate at which protostellar cores have been
misclassified as starless cores calculated as <1/56, or < 2%. We use synthetic
observations to show that starless cores collapsing following the turbulent
fragmentation scenario are detectable by our ALMA observations when their
central densities exceed ~10^8 cm^-3, with the exact density dependent on the
viewing geometry. Bonnor-Ebert spheres, on the other hand, remain undetected to
central densities at least as high as 10^10 cm^-3. Our starless core
non-detections are used to infer that either the star formation rate is
declining in Chamaeleon I and most of the starless cores are not collapsing,
matching the findings of previous studies, or that the evolution of starless
cores are more accurately described by models that develop less substructure
than predicted by the turbulent fragmentation scenario, such as Bonnor-Ebert
spheres. We outline future work necessary to distinguish between these two
possibilities.Comment: Accepted by Ap
The Formation of Low-Mass Binary Star Systems Via Turbulent Fragmentation
We characterize the infall rate onto protostellar systems forming in
self-gravitating radiation-hydrodynamic simulations. Using two dimensionless
parameters to determine disks' susceptability to gravitational fragmentation,
we infer limits on protostellar system multiplicity and the mechanism of binary
formation. We show that these parameters give robust predictions even in the
case of marginally resolved protostellar disks. We find that protostellar
systems with radiation feedback predominately form binaries via turbulent
fragmentation, not disk instability, and we predict turbulent fragmentation is
the dominant channel for binary formation for low-mass stars. We clearly
demonstrate that systems forming in simulations including radiative feedback
have fundamentally different parameters than those in purely hydrodynamic
simulations.Comment: 11 pages, 10 figures, accepted to Ap
Deuteration as an evolutionary tracer in massive-star formation
Theory predicts, and observations confirm, that the column density ratio of a
molecule containing D to its counterpart containing H can be used as an
evolutionary tracer in the low-mass star formation process. Since it remains
unclear if the high-mass star formation process is a scaled-up version of the
low-mass one, we investigated whether the relation between deuteration and
evolution can be applied to the high-mass regime. With the IRAM-30m telescope,
we observed rotational transitions of N2D+ and N2H+ and derived the deuterated
fraction in 27 cores within massive star-forming regions understood to
represent different evolutionary stages of the massive-star formation process.
Results. Our results clearly indicate that the abundance of N2D+ is higher at
the pre-stellar/cluster stage, then drops during the formation of the
protostellar object(s) as in the low-mass regime, remaining relatively constant
during the ultra-compact HII region phase. The objects with the highest
fractional abundance of N2D+ are starless cores with properties very similar to
typical pre-stellar cores of lower mass. The abundance of N2D+ is lower in
objects with higher gas temperatures as in the low-mass case but does not seem
to depend on gas turbulence. Our results indicate that the N2D+-to-N2H+ column
density ratio can be used as an evolutionary indicator in both low- and
high-mass star formation, and that the physical conditions influencing the
abundance of deuterated species likely evolve similarly during the processes
that lead to the formation of both low- and high-mass stars.Comment: Accepted by A&AL, 4 pages, 2 figures, 2 appendices (one for Tables,
one for additional figures
The properties of SCUBA cores in the Perseus molecular cloud: the bias of clump-finding algorithms
We present a new analysis of the properties of star-forming cores in the
Perseus molecular cloud, identified in SCUBA 850 micron data. Our goal is to
determine which core properties can be robustly identified and which depend on
the extraction technique. Four regions in the cloud are examined: NGC1333,
IC348/HH211, L1448 and L1455. We identify clumps of dust emission using two
popular automated algorithms, CLFIND and GAUSSCLUMPS, finding 85 and 122 clumps
in total respectively. Some trends are true for both populations: clumps become
increasingly elongated over time and are consistent with constant surface
brightness objects, with an average brightness ~4 to 10 times larger than the
surrounding molecular cloud; the clump mass distribution (CMD) resembles the
stellar intial mass function, with a slope alpha = -2.0+/-0.1 for CLFIND and
alpha = -3.15+/-0.08 for GAUSSCLUMPS, which straddle the Salpeter value. The
mass at which the slope shallows (similar for both algorithms at M~6 Msun)
implies a star-forming efficiency of between 10 and 20 per cent. Other trends
reported elsewhere depend on the clump-finding technique: we find protostellar
clumps are both smaller (for GAUSSCLUMPS) and larger (for CLFIND) than their
starless counterparts; the functional form, best-fitting to the CMD, is
different for the two algorithms. The GAUSSCLUMPS CMD is best-fitted with a
log-normal distribution, whereas a broken power law is best for CLFIND; the
reported lack of massive starless cores in previous studies can be seen in the
CLFIND but not the GAUSSCLUMPS data. Our approach highlights similarities and
differences between the clump populations, illustrating the caution that must
be exercised when comparing results from different studies and interpreting the
properties of continuum cores.Comment: 19 pages, 17 figures, accepted for publication by MNRA
A submillimetre survey of the kinematics of the Perseus molecular cloud - III. Clump kinematics
We explore the kinematics of continuum clumps in the Perseus molecular cloud,
derived from C18O J=3-2 data. Two populations are examined, identified using
the automated algorithms CLFIND and GAUSSCLUMPS on existing SCUBA data. The
clumps have supersonic linewidths with distributions which suggest the C18O
line probes a lower-density 'envelope' rather than a dense inner core. Similar
linewidth distributions for protostellar and starless clumps implies protostars
do not have a significant impact on their immediate environment. The proximity
to an active young stellar cluster seems to affect the linewidths: those in
NGC1333 are greater than elsewhere. In IC348 the proximity to the old IR
cluster has little influence, with the linewidths being the smallest of all. A
virial analysis suggests that the clumps are bound and close to equipartition.
In particular, the starless clumps occupy the same parameter space as the
protostars, suggesting they are true stellar precursors and will go on to form
stars. We also search for ordered C18O velocity gradients across the face of
each core, usually interpreted as rotation. We note a correlation between the
directions of the identified gradients and outflows across protostars,
indicating we may not have a purely rotational signature. The fitted gradients
are larger than found in previous work, probably as a result of the higher
resolution of our data and/or outflow contamination. These gradients, if
interpreted solely in terms of rotation, suggest that rotation is not
dynamically significant. Furthermore, derived specific angular momenta are
smaller than observed in previous studies, centred around j~0.001 km/s pc,
which indicates we have identified lower levels of rotation, or that the C18O
J=3-2 line probes conditions significantly denser and/or colder than n~10^5 per
cc and T~10 K.Comment: 20 pages, 20 figures, accepted for publication by MNRAS.
Supplementary, on-line only material available from
http://www.mrao.cam.ac.uk/~eic22/Papers/CR10b_suppmaterial.pd
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