45 research outputs found
Comparing complex impedance and bias step measurements of Simons Observatory transition edge sensors
The Simons Observatory (SO) will perform ground-based observations of the
cosmic microwave background (CMB) with several small and large aperture
telescopes, each outfitted with thousands to tens of thousands of
superconducting aluminum manganese (AlMn) transition-edge sensor bolometers
(TESs). In-situ characterization of TES responsivities and effective time
constants will be required multiple times each observing-day for calibrating
time-streams during CMB map-making. Effective time constants are typically
estimated in the field by briefly applying small amplitude square-waves on top
of the TES DC biases, and fitting exponential decays in the bolometer response.
These so-called "bias step" measurements can be rapidly implemented across
entire arrays and therefore are attractive because they take up little
observing time. However, individual detector complex impedance measurements,
while too slow to implement during observations, can provide a fuller picture
of the TES model and a better understanding of its temporal response. Here, we
present the results of dark TES characterization of many prototype SO
bolometers and compare the effective thermal time constants measured via bias
steps to those derived from complex impedance data.Comment: 10 pages, 6 figures, SPIE Astronomical Telescopes + Instrumentation
2020, Paper Number: 11453-18
Instrumental performance and results from testing of the BLAST-TNG receiver, submillimeter optics, and MKID arrays
Polarized thermal emission from interstellar dust grains can be used to map
magnetic fields in star forming molecular clouds and the diffuse interstellar
medium (ISM). The Balloon-borne Large Aperture Submillimeter Telescope for
Polarimetry (BLASTPol) flew from Antarctica in 2010 and 2012 and produced
degree-scale polarization maps of several nearby molecular clouds with
arcminute resolution. The success of BLASTPol has motivated a next-generation
instrument, BLAST-TNG, which will use more than 3000 linear polarization
sensitive microwave kinetic inductance detectors (MKIDs) combined with a 2.5m
diameter carbon fiber primary mirror to make diffraction-limited observations
at 250, 350, and 500 m. With 16 times the mapping speed of BLASTPol,
sub-arcminute resolution, and a longer flight time, BLAST-TNG will be able to
examine nearby molecular clouds and the diffuse galactic dust polarization
spectrum in unprecedented detail. The 250 m detector array has been
integrated into the new cryogenic receiver, and is undergoing testing to
establish the optical and polarization characteristics of the instrument.
BLAST-TNG will demonstrate the effectiveness of kilo-pixel MKID arrays for
applications in submillimeter astronomy. BLAST-TNG is scheduled to fly from
Antarctica in December 2017 for 28 days and will be the first balloon-borne
telescope to offer a quarter of the flight for "shared risk" observing by the
community.Comment: Presented at SPIE Millimeter, Submillimeter, and Far-Infrared
Detectors and Instrumentation for Astronomy VIII, June 29th, 201
The Balloon-Borne Large Aperture Submillimeter Telescope Observatory
The BLAST Observatory is a proposed superpressure balloon-borne polarimeter
designed for a future ultra-long duration balloon campaign from Wanaka, New
Zealand. To maximize scientific output while staying within the stringent
superpressure weight envelope, BLAST will feature new 1.8m off-axis optical
system contained within a lightweight monocoque structure gondola. The payload
will incorporate a 300L He cryogenic receiver which will cool 8,274
microwave kinetic inductance detectors (MKIDs) to 100mK through the use of an
adiabatic demagnetization refrigerator (ADR) in combination with a He
sorption refrigerator all backed by a liquid helium pumped pot operating at 2K.
The detector readout utilizes a new Xilinx RFSOC-based system which will run
the next-generation of the BLAST-TNG KIDPy software. With this instrument we
aim to answer outstanding questions about dust dynamics as well as provide
community access to the polarized submillimeter sky made possible by
high-altitude observing unrestricted by atmospheric transmission. The BLAST
Observatory is designed for a minimum 31-day flight of which 70 will be
dedicated to observations for BLAST scientific goals and the remaining 30
will be open to proposals from the wider astronomical community through a
shared-risk proposals program.Comment: Presented at SPIE Ground-based and Airborne Telescopes VIII, December
13-18, 202
Characterization, deployment, and in-flight performance of the BLAST-TNG cryogenic receiver
The Next Generation Balloon-borne Large Aperture Submillimeter Telescope
(BLAST-TNG) is a submillimeter polarimeter designed to map interstellar dust
and galactic foregrounds at 250, 350, and 500 microns during a 24-day Antarctic
flight. The BLAST-TNG detector arrays are comprised of 918, 469, and 272 MKID
pixels, respectively. The pixels are formed from two orthogonally oriented,
crossed, linear-polarization sensitive MKID antennae. The arrays are cooled to
sub 300mK temperatures and stabilized via a closed cycle He sorption fridge
in combination with a He vacuum pot. The detectors are read out through a
combination of the second-generation Reconfigurable Open Architecture Computing
Hardware (ROACH2) and custom RF electronics designed for BLAST-TNG. The
firmware and software designed to readout and characterize these detectors was
built from scratch by the BLAST team around these detectors, and has been
adapted for use by other MKID instruments such as TolTEC and OLIMPO. We present
an overview of these systems as well as in-depth methodology of the
ground-based characterization and the measured in-flight performance.Comment: Presented at SPIE Millimeter, Submillimeter, and Far-Infrared
Detectors and Instrumentation for Astronomy X, December 13-18, 202
The Simons Observatory Large Aperture Telescope Receiver
The Simons Observatory (SO) Large Aperture Telescope Receiver (LATR) will be
coupled to the Large Aperture Telescope located at an elevation of 5,200 m on
Cerro Toco in Chile. The resulting instrument will produce arcminute-resolution
millimeter-wave maps of half the sky with unprecedented precision. The LATR is
the largest cryogenic millimeter-wave camera built to date with a diameter of
2.4 m and a length of 2.6 m. It cools 1200 kg of material to 4 K and 200 kg to
100 mk, the operating temperature of the bolometric detectors with bands
centered around 27, 39, 93, 145, 225, and 280 GHz. Ultimately, the LATR will
accommodate 13 40 cm diameter optics tubes, each with three detector wafers and
a total of 62,000 detectors. The LATR design must simultaneously maintain the
optical alignment of the system, control stray light, provide cryogenic
isolation, limit thermal gradients, and minimize the time to cool the system
from room temperature to 100 mK. The interplay between these competing factors
poses unique challenges. We discuss the trade studies involved with the design,
the final optimization, the construction, and ultimate performance of the
system