295 research outputs found
MUSTANG 3.3 Millimeter Continuum Observations of Class 0 Protostars
We present observations of six Class 0 protostars at 3.3 mm (90 GHz) using
the 64-pixel MUSTANG bolometer camera on the 100-m Green Bank Telescope. The
3.3 mm photometry is analyzed along with shorter wavelength observations to
derive spectral indices (S_nu ~ nu^alpha) of the measured emission. We utilize
previously published dust continuum radiative transfer models to estimate the
characteristic dust temperature within the central beam of our observations. We
present constraints on the millimeter dust opacity index, beta, between 0.862
mm, 1.25 mm, and 3.3 mm. Beta_mm typically ranges from 1.0 to 2.4 for Class 0
sources. The relative contributions from disk emission and envelope emission
are estimated at 3.3 mm. L483 is found to have negligible disk emission at 3.3
mm while L1527 is dominated by disk emission within the central beam. The
beta_mm^disk <= 0.8 - 1.4 for L1527 indicates that grain growth is likely
occurring in the disk. The photometry presented in this paper may be combined
with future interferometric observations of Class 0 envelopes and disks.Comment: 19 pages, 3 figures, AJ accepted, in pres
Galaxy Cluster Pressure Profiles as Determined by Sunyaev Zel'dovich Effect Observations with MUSTANG and Bolocam I: Joint Analysis Technique
We present a technique to constrain galaxy cluster pressure profiles by
jointly fitting Sunyaev-Zel'dovich effect (SZE) data obtained with MUSTANG and
Bolocam for the clusters Abell 1835 and MACS0647. Bolocam and MUSTANG probe
different angular scales and are thus highly complementary. We find that the
addition of the high resolution MUSTANG data can improve constraints on
pressure profile parameters relative to those derived solely from Bolocam. In
Abell 1835 and MACS0647, we find gNFW inner slopes of and , respectively when
and are constrained to 0.86 and 4.67 respectively. The fitted
SZE pressure profiles are in good agreement with X-ray derived pressure
profiles.Comment: 12 pages, 12 figures. Submitted to Ap
Confirming the Primarily Smooth Structure of the Vega Debris Disk at Millimeter Wavelengths
Clumpy structure in the debris disk around Vega has been previously reported at millimeter wavelengths and attributed to concentrations of dust grains trapped in resonances with an unseen planet. However, recent imaging at similar wavelengths with higher sensitivity has disputed the observed structure. We present three new millimeter wavelength observations that help to resolve the puzzling and contradictory observations. We have observed the
Vega system with the Submillimeter Array (SMA) at a wavelength of 880 μm and an angular resolution of 5"; with the Combined Array for Research in Millimeter-wave Astronomy (CARMA) at a wavelength of 1.3 mm and
an angular resolution of 5"; and with the Green Bank Telescope (GBT) at a wavelength of 3.3 mm and angular resolution of 10". Despite high sensitivity and short baselines, we do not detect the Vega debris disk in either of the
interferometric data sets (SMA and CARMA), which should be sensitive at high significance to clumpy structure based on previously reported observations. We obtain a marginal (3σ) detection of disk emission in the GBT data;
the spatial distribution of the emission is not well constrained.We analyze the observations in the context of several different models, demonstrating that the observations are consistent with a smooth, broad, axisymmetric disk with inner radius 20–100 AU and width ≾50 AU. The interferometric data require that at least half of the 860 μm emission detected by previous single-dish observations with the James Clerk Maxwell Telescope be distributed axisymmetrically, ruling out strong contributions from flux concentrations on spatial scales of ≾100 AU. These observations support recent results from the Plateau de Bure Interferometer indicating that previous detections of clumpy structure in the Vega debris disk were spurious
Simons Observatory: Broadband Metamaterial Anti-Reflection Cuttings for Large Aperture Alumina Optics
We present the design, fabrication, and measured performance of metamaterial
Anti-Reflection Cuttings (ARCs) for large-format alumina filters operating over
more than an octave of bandwidth to be deployed on the Simons Observatory (SO).
The ARC consists of sub-wavelength features diced into the optic's surface
using a custom dicing saw with near-micron accuracy. The designs achieve
percent-level control over reflections at angles of incidence up to 20.
The ARCs were demonstrated on four 42 cm diameter filters covering the 75-170
GHz band and a 50 mm diameter prototype covering the 200-300 GHz band. The
reflection and transmission of these samples were measured using a broadband
coherent source that covers frequencies from 20 GHz to 1.2 THz. These
measurements demonstrate percent-level control over reflectance across the
targeted pass-bands and a rapid reduction in transmission as the wavelength
approaches the length scale of the metamaterial structure where scattering
dominates the optical response. The latter behavior enables the use of the
metamaterial ARC as a scattering filter in this limit.Comment: 9 pages, 8 figures, submitted to Applied Optic
A Bright Submillimeter Source in the Bullet Cluster (1E0657--56) Field Detected with BLAST
We present the 250, 350, and 500 micron detection of bright submillimeter
emission in the direction of the Bullet Cluster measured by the Balloon-borne
Large Aperture Submillimeter Telescope (BLAST). The 500 micron centroid is
coincident with an AzTEC 1.1 mm point-source detection at a position close to
the peak lensing magnification produced by the cluster. However, the 250 micron
and 350 micron centroids are elongated and shifted toward the south with a
differential shift between bands that cannot be explained by pointing
uncertainties. We therefore conclude that the BLAST detection is likely
contaminated by emission from foreground galaxies associated with the Bullet
Cluster. The submillimeter redshift estimate based on 250-1100 micron
photometry at the position of the AzTEC source is z_phot = 2.9 (+0.6 -0.3),
consistent with the infrared color redshift estimation of the most likely IRAC
counterpart. These flux densities indicate an apparent far-infrared luminosity
of L_FIR = 2E13 Lsun. When the amplification due to the gravitational lensing
of the cluster is removed, the intrinsic far-infrared luminosity of the source
is found to be L_FIR <= 10^12 Lsun, consistent with typical luminous infrared
galaxies.Comment: Accepted for publication in the Astrophysical Journal. Maps are
available at http://blastexperiment.info
The Atacama Large Aperture Submillimetre Telescope (AtLAST)
The coldest and densest structures of gas and dust in the Universe have
unique spectral signatures across the (sub-)millimetre bands (~GHz). The current generation of single dish facilities has given a
glimpse of the potential for discovery, while sub-mm interferometers have
presented a high resolution view into the finer details of known targets or in
small-area deep fields. However, significant advances in our understanding of
such cold and dense structures are now hampered by the limited sensitivity and
angular resolution of our sub-mm view of the Universe at larger scales.
In this context, we present the case for a new transformational astronomical
facility in the 2030s, the Atacama Large Aperture Submillimetre Telescope
(AtLAST). AtLAST is a concept for a 50-m-class single dish telescope, with a
high throughput provided by a 2~deg - diameter Field of View, located on a
high, dry site in the Atacama with good atmospheric transmission up to ~THz, and fully powered by renewable energy.
We envision AtLAST as a facility operated by an international partnership
with a suite of instruments to deliver the transformative science that cannot
be achieved with current or in-construction observatories. As an 50m-diameter
telescope with a full complement of advanced instrumentation, including highly
multiplexed high-resolution spectrometers, continuum cameras and integral field
units, AtLAST will have mapping speeds hundreds of times greater than current
or planned large aperture ( 12m) facilities. By reaching confusion limits
below L in the distant Universe, resolving low-mass protostellar cores at
the distance of the Galactic Centre, and directly mapping both the cold and the
hot (the Sunyaev-Zeldovich effect) circumgalactic medium of galaxies, AtLAST
will enable a fundamentally new understanding of the sub-mm Universe.Comment: 20 pages, 5 figures, to be submitted to SPIE Astronomical telescopes
& Instruments 2020, Ground-based and Airborne Telescopes VIII (conference
11445, abstract 290
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