SPIDER: a balloon-borne CMB polarimeter for large angular scales
ABSTRACT We describe SPIDER, a balloon-borne instrument to map the polarization of the
millimeter-wave sky with degree angular resolution. Spider consists of six
monochromatic refracting telescopes, each illuminating a focal plane of
large-format antenna-coupled bolometer arrays. A total of 2,624 superconducting
transition-edge sensors are distributed among three observing bands centered at
90, 150, and 280 GHz. A cold half-wave plate at the aperture of each telescope
modulates the polarization of incoming light to control systematics. Spider's
first flight will be a 20-30-day Antarctic balloon campaign in December 2011.
This flight will map \sim8% of the sky to achieve unprecedented sensitivity to
the polarization signature of the gravitational wave background predicted by
inflationary cosmology. The Spider mission will also serve as a proving ground
for these detector technologies in preparation for a future satellite mission.
- SourceAvailable from: William Jones[Show abstract] [Hide abstract]
ABSTRACT: We present the technology and control methods developed for the pointing system of the SPIDER experiment. SPIDER is a balloon-borne polarimeter designed to detect the imprint of primordial gravitational waves in the polarization of the Cosmic Microwave Background radiation. We describe the two main components of the telescope's azimuth drive: the reaction wheel and the motorized pivot. A 13 kHz PI control loop runs on a digital signal processor, with feedback from fibre optic rate gyroscopes. This system can control azimuthal speed with < 0.02 deg/s RMS error. To control elevation, SPIDER uses stepper-motor-driven linear actuators to rotate the cryostat, which houses the optical instruments, relative to the outer frame. With the velocity in each axis controlled in this way, higher-level control loops on the onboard flight computers can implement the pointing and scanning observation modes required for the experiment. We have accomplished the non-trivial task of scanning a 5000 lb payload sinusoidally in azimuth at a peak acceleration of 0.8 deg/s$^2$, and a peak speed of 6 deg/s. We can do so while reliably achieving sub-arcminute pointing control accuracy.07/2014;
- [Show abstract] [Hide abstract]
ABSTRACT: SPIDER is a balloon-borne instrument designed to map the polarization of the cosmic microwave background (CMB) with degree-scale resolution over a large fraction of the sky. SPIDER's main goal is to measure the amplitude of primordial gravitational waves through their imprint on the polarization of the CMB if the tensor-to-scalar ratio, r, is greater than 0.03. To achieve this goal, instrumental systematic errors must be controlled with unprecedented accuracy. Here, we build on previous work to use simulations of SPIDER observations to examine the impact of several systematic effects that have been characterized through testing and modeling of various instrument components. In particular, we investigate the impact of the non-ideal spectral response of the half-wave plates, coupling between focal-plane components and Earth's magnetic field, and beam mismatches and asymmetries. We also present a model of diffuse polarized foreground emission based on a three-dimensional model of the Galactic magnetic field and dust, and study the interaction of this foreground emission with our observation strategy and instrumental effects. We find that the expected level of foreground and systematic contamination is sufficiently low for SPIDER to achieve its science goals.The Astrophysical Journal 08/2011; 738(1):63. · 6.28 Impact Factor
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ABSTRACT: We propose a high thermal conductivity infra-red (IR) filters using alumina for use in a millimeter wave detection. We construct a prototype two-layer anti-reflection-coated alumina filter with a diameter of 100 mm and a thickness of 2 mm, and characterize its thermal and optical properties. The transmittance of this filter at the millimeter wave for 95 GHz and 150 GHz is 97 % and 95 % while the estimated 3 dB cutoff frequency is at 450 GHz. The high thermal conductivity of alumina minimizes thermal gradient. We measure the differential temperature of only 0.21 K between the center and the edge of the filter when it is mounted on a thermal anchor of 77 K. We also construct the thermal model based on the prototype filter and analyze the scalability of a filter diameter. We conclude that temperature increase at the center of alumina IR filter is less than 6 K even with a large diameter of 500 mm, when the temperature at the edge of the filter is 50 K. This is suitable for an application to a large-throughput next-generation CMB polarization experiment, such as POLARBEAR-2 (PB-2).Applied Optics 11/2013; 53(9). · 1.69 Impact Factor
Spider: a balloon-borne CMB
polarimeter for large angular scales
J.P. Filippinia*, P.A.R. Adeb, M. Amiric, S.J. Bentond, R. Biharye, J.J. Bocka,f, J.R. Bondg,
J.A. Bonettif, S.A. Bryane, B. Burgerc, H.C. Chiangh, C.R. Contaldii, B.P. Crilla,f, O. Dor´ ea,f,
M. Farhangd, L.M. Fisseld, N.N. Gandilod, S.R. Golwalaa, J.E. Gudmundssonh, M. Halpernc,
M. Hasselfieldc, G. Hiltonj, W. Holmesf, V.V. Hristova, K.D. Irwinj, W.C. Jonesh, C.L. Kuok,
C.J. MacTavishl, P.V. Masona, T.E. Montroye, T.A. Morforda, C.B. Netterfieldd, D.T. O’Deai,
A.S. Rahlinh, C.D. Reintsemaj, J.E. Ruhle, M.C. Runyana, M.A. Schenkera, J.A. Shariffd,
J.D. Solerd, A. Trangsruda, C. Tuckerb, R.S. Tuckera, and A.D. Turnerf
aDivision of Physics, Mathematics, and Astronomy, California Institute of Technology,
Pasadena, CA, USA;
bSchool of Physics and Astronomy, Cardiff University, Cardiff, UK;
cDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC,
dDepartment of Physics, University of Toronto, Toronto, ON, Canada;
eDepartment of Physics, Case Western Reserve University, Cleveland, OH, USA;
fJet Propulsion Laboratory, Pasadena, CA, USA;
gCanadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON, Canada;
hDepartment of Physics, Princeton University, Princeton, NJ, USA;
iDepartment of Physics, Imperial College, University of London, London, UK;
jNational Institute of Standards and Technology, Boulder, CO, USA;
kDepartment of Physics, Stanford University, Stanford, CA, USA;
lKavli Institute for Cosmology, University of Cambridge, Cambridge, UK
We describe Spider, a balloon-borne instrument to map the polarization of the millimeter-wave sky with degree
angular resolution. Spider consists of six monochromatic refracting telescopes, each illuminating a focal plane
of large-format antenna-coupled bolometer arrays. A total of 2,624 superconducting transition-edge sensors are
distributed among three observing bands centered at 90, 150, and 280 GHz. A cold half-wave plate at the
aperture of each telescope modulates the polarization of incoming light to control systematics. Spider’s first
flight will be a 20-30-day Antarctic balloon campaign in December 2011. This flight will map ∼8% of the sky to
achieve unprecedented sensitivity to the polarization signature of the gravitational wave background predicted
by inflationary cosmology. The Spider mission will also serve as a proving ground for these detector technologies
in preparation for a future satellite mission.
Keywords: Spider, cosmic microwave background, polarization, inflation, transition-edge sensor
Over the past 45 years, observations of the cosmic microwave background (CMB) have transformed our under-
standing of the universe. The discovery of this primordial radiation field1heralded the triumph of the hot Big
Bang theory, laying down a timeline for cosmological history. The discovery of tiny (one part in 105) fluctuations
in the temperature of this radiation across the sky2gave cosmologists a snapshot of the birth of large-scale
*Corresponding author; E-mail: firstname.lastname@example.org, Tel: 1 626 395 2601
arXiv:1106.2158v1 [astro-ph.CO] 10 Jun 2011
structure in our universe, as well as evidence that its history began with an inflationary epoch of rapid expan-
sion. More recently, a series of terrestrial, balloon-borne, and satellite instruments have taken advantage of rapid
advances in millimeter-wave technology to map these anisotropies with ever greater fidelity. These measurements
continue to provide an ever-more-precise picture of the contents, geometry, and history of the cosmos.3
The next frontier of this endeavor is the measurement of the tiny degree of polarization in the microwave
background radiation. Thomson scattering at the epoch of recombination transformed quadrupole anisotropies
in the photon-baryon fluid into a slight polarization in the CMB, with an intensity more than an order of
magnitude smaller than that of the temperature anisotropies. The pattern of this polarization across the sky
encodes information about the local conditions within the last-scattering surface that is complementary to that
available in the temperature anisotropies. Early measurements of CMB polarization have already provided
independent confirmation of our understanding of recombination and improved our estimates of cosmological
In addition to improved constraints on existing cosmological parameters, future precision measurements of
CMB polarization promise qualitatively new information about the history of our universe. The large-scale po-
larization pattern encodes unique data on two epochs of cosmological history that have thus far been hidden from
observation: the reionization of the universe by the ignition of the first stars, and the inflationary period of rapid
expansion in the first ∼10−33second after the Big Bang. Reionization generates new opportunities for Thomson
scattering of CMB photons, and thus generates additional polarization of the microwave sky. The history of
reionization is thus encoded in the CMB polarization pattern on the very largest angular scales, easily distin-
guished from the signatures of recombination at smaller angular scales. Gravitational waves generated during the
inflationary era induce polarization during the recombination and reionization epochs. These gravitational waves
are unique in their ability to generate a “B-mode” polarization pattern at large angular scales, distinguishable
from the more common “E-mode” pattern by its opposite transformation under spatial inversion.6The detec-
tion of a B-mode pattern on large angular scales would be a dramatic confirmation of the inflationary theory
of cosmology. The CMB polarization pattern also holds valuable information about more recent cosmological
history, encoded in the distortion of the primordial polarization map by gravitational lensing.
In this paper we describe Spider, a balloon-borne telescope array optimized to search for the signature of
cosmic inflation in the polarization of the CMB. Spider will take advantage of massively multiplexed bolometer
arrays and a vantage point above the bulk of the atmosphere to map the polarization of the millimeter-wave sky
with higher fidelity than any CMB receiver to date. The instrument and its scan strategy are optimized to map
a large fraction of the sky at degree angular scales, an ideal approach for a targeted search for the “B-mode”
signature of inflation. Spider will use stepped half-wave plates and broad frequency coverage to achieve excellent
control of instrumental systematics and contamination from galactic foregrounds. Following in the tradition of
BOOMERanG and BLAST, Spider will also serve as a technology pathfinder for a satellite mission to make
definitive maps of CMB polarization.
The Spider instrument has previously been described by Montroy et al.7and Crill et al.8in this conference
series. MacTavish et al.9have presented a detailed study of instrumental systematics for Spider, focusing on
the case of a 2-6 day flight from Alice Springs, Australia. In this work we describe the present status of Spider,
which is currently targeting an Antarctic flight during the 2011-12 austral summer. Three other contributions
to these proceedings describe particular subsystems of Spider in greater detail: Bryan et al.,10Gudmundsson
et al.,11and Runyan et al.12
2. SCIENTIFIC GOALS
The primary goal of the Spider project is to search for the signature of a primordial gravitational wave back-
ground in the polarization of the cosmic microwave background, a key prediction of the inflationary paradigm
of cosmogenesis. To this end, Spider will map the polarization of the millimeter sky with high fidelity on the
largest scales allowed by the presence of Galactic emission. The Spider polarization map will also address two
secondary science goals, also of great scientific importance: measurement of the weak lensing of the CMB by
cosmological structure and characterization of polarized emission from interstellar dust at high galactic latitudes.
The raw sensitivity of its receivers and the excellent control of systematics afforded by its instrument design will
give Spider’s data set lasting value.
? l (l+1)/2 ? Cl [nKcmb]
? l (l+1)/2 ? Cl [nKcmb]
Figure 1. An illustration of the B-mode angular power spectra and the noise levels associated with the WMAP 8-year,
Planck, and Spider surveys. The left panel shows the theoretical spectra for the E-modes (labelled EE), gravitational
lensing B-modes (labelled BBlensing), and inflationary gravitational wave B-modes (labelled BBGW) for r = 0.1. The
right panel overlays the noise thresholds per multipole (including both statistical noise and sample variance) for the three
surveys. The curves for WMAP and Planck are derived from a simple Fisher analysis. For Spider, the Fisher errors
are corrected for instrumental effects using ensembles of time domain simulations that include the scan strategy, noise
correlations, and stationarity boundaries. The line for Spider has been truncated at a multipole of ten as the limited
sky coverage of an Antarctic flight will prevent us from probing larger scales. The effects of foreground emission are not
included in these results; in particular, it is possible that foreground emission will limit Planck’s measurement of the low-?
BB bump induced by reionization.
Figure 2. At left: the tensor to scalar likelihood, in the limit of a small tensor to scalar ratio (r = 0.001, for Spider and
Planck with and without including the impact of foregrounds. At right: the same, for the case of a relatively high tensor to
scalar ratio, r = 0.12, corresponding to a simple slow roll inflation (m2φ2). Both assume an optical depth to reionization
of τ = 0.09. Planck’s ability to measure or place limits on r is due entirely to the B-mode signature coming from the
epoch of reionization on angular scales larger than ∼ 10◦, where Galactic foregrounds are dominant. The dramatic impact
of these foregrounds on Planck’s r measurement are evident.
2.1 The echoes of inflation
Models of inflation13postulate that the universe underwent a period of extremely rapid expansion during its
first moments, increasing in scale by a factor of ?1025in a mere ∼10−33second. This massive expansion left
the universe nearly spatially-flat and remarkably homogeneous and isotropic on its largest scales. Quantum
fluctuations in the “inflaton” field (or fields) that caused this expansion seeded tiny inhomogeneities into the
universe’s energy density. Over time these ripples grew under their own gravity, eventually evolving into the
large-scale structures of the modern universe. Though this basic picture has passed every observational test to
date, the identity of the inflaton field that started it all remains unknown. The particle physics behind inflation is
likely to occur at energy scales far above those accessible to particle accelerators, so cosmological measurements
are our primary avenue for investigating inflationary physics.
A unique prediction of inflation is that these quantum fluctuations should have seeded the early universe
with both scalar and tensor perturbations of the underlying spatial metric over a wide range of distance scales.
The former grew into the large-scale structure we observe today; the latter manifested themselves as a stochastic
background of gravitational waves. The long wavelengths of these primordial gravitational waves render them
essentially undetectable today (at least with near-term technology), but their presence at the epoch of recombi-
nation would have imparted a unique signature to the polarization of the CMB: a B-mode contribution peaking
at angular scales of a few degrees (? ≈ 80).14–16Both tensor and scalar perturbations generate polarization
through the same mechanism (Thomson scattering), but symmetry requires that scalar perturbations generate
only E-modes, while tensor perturbations generate a mixture of both. Though gravitational lensing can convert
E-modes to B-modes on sub-degree angular scales, no process in nature is expected to produce a B-mode signal
on larger scales. A detection of a B-mode component on large angular scales would thus be a clear confirmation
that our universe began with an inflationary epoch.
The power in the inflationary gravitational waves relative to that in the usual scalar anisotropies is charac-
terized by the tensor-to-scalar ratio, r. Current cosmological data constrain r relatively weakly: r ? 0.20 at
the 95% confidence level, with some dependence on cosmological assumptions.3The value of r is a function of
the energy scale of the new physical processes behind inflation (Einf), a scale which is not well constrained by
theory. A priori, Einf could lie anywhere between the TeV scale of current accelerator data and the Planck
scale (1019GeV), and over most of this range the inflationary B-mode signal will be undetectable amidst the
background from gravitational lensing of E-modes. If inflation is associated with the physics of Grand Unified
Theories (GUTs), however, its B-mode signature may be detectable: r ? 0.01 corresponds to Einf? 1016GeV.
Recent evidence that the spectral index of the primordial power spectrum is less than unity (ns= 0.96 ± 0.1 as
of this writing3) provides tantalizing support for this hypothesis: in many of the simplest single-field inflation
models, a low spectral index corresponds to detectably large values of r.17If an inflationary B-mode patten
is detected, it will provide invaluable information about the nature of inflation and the fundamental physics
responsible for it.
Figure 1 shows theoretical power spectra for the E-mode and B-mode polarization components, under the
assumption that r = 0.1. The inflationary contribution to the B-mode spectrum peaks at angular scales of a
few degrees (?∼80). At smaller scales this signal is contaminated by the gravitational lensing of E-modes; at the
largest scales one cannot avoid galactic foregrounds. This suggests a clear strategy for a targeted measurement
of r: a suborbital mission to map the CMB polarization with extremely high fidelity on relatively large angular
scales (10 ? ? ? 300). Spider is designed to implement this strategy, combining simple degree-scale optics
with the low foregrounds and large sky coverage afforded by Antarctic ballooning. This strategy is extremely
complementary to that of Planck, which achieves its sensitivity to r solely from the lowest-? reionization peak
in the B-mode spectrum. Figure 2 compares the predicted effect of galactic foregrounds on each experiment’s
sensitivity to r. Though the two instruments have comparable raw sensitivities to r, Spider’s reach is hampered
far less by the introduction of galactic foregrounds. Spider is designed to measure the tensor-to-scalar ratio
corresponding to single-field inflationary models near the GUT scale, or to experimentally rule them out by
setting an interesting upper limit r < 0.03 (at 3σ).
2.2 Weak lensing of the microwave background
As the CMB radiation propagates from the surface of last scattering to our telescope, it is lensed by the gravi-
tational potential it traverses. Such lensing distorts the polarization pattern we observe in the sky, converting
a small portion of the E-mode power into a B-mode signal. Though this lensing B-mode (shown in Figure 1)
constitutes a limiting background to searches for a primordial B-signal, it is also a valuable probe of cosmology
in its own right. Through lensing, the B-mode polarization of the CMB is a sensitive probe of the matter power
spectrum, and thus on such parameters as the dark energy equation and the sum of the neutrino masses.18,19
The great depth of Spider’s polarization maps will allow it to probe the lensing of the CMB polarization field,
with an anticipated signal-to-noise per multipole on the lensing signal (e.g. for r = 0) of order unity from
10 < ? < 300 (see Figure 1).
2.3 Galactic dust emission
Confusion with galactic foregrounds is likely to set the ultimate limit on measurements of CMB polarization
on large angular scales. WMAP has mapped the polarization of galactic synchrotron emission,20the dominant
CMB foreground below ∼100 GHz, but the polarized contribution of dust emission at higher frequencies is not
well constrained. Spider will map the polarized emission of dust at high galactic latitude, providing valuable
insight into the denser portions of the interstellar medium. Spider’s high-fidelity polarized dust maps will
complement the all-sky maps produced by the Planck satellite, which will provide a precise determination of
the overall intensity of dust emission. The 280 GHz band of the Spider instrument is very complementary to
Planck’s frequency coverage, bridging the gap between the latter’s bands at 217 GHz and and 353 GHz.
Spider’s maiden voyage will be a long-duration balloon flight from McMurdo station, Antarctica, during the
2011-12 austral summer. Due to the persistent daylight the instrument will scan in azimuth, with an amplitude
of 45 degrees and a maximum azimuthal velocity of 6 degrees/second. The scan elevation will be changed by 0.5
degrees each hour, covering the range between 28 and 40 degrees each day. The half-wave plate will be operated
in a stepped mode, turning by a discrete number of degrees several times each day. The sky coverage of this
strategy is enhanced by Spider’s small, easily-shielded aperture, which allows it to scan closer to the sun than
previous suborbital instruments such as BOOMERanG or EBEX.
Figure 3 illustrates the expected sky coverage from this scan strategy and compares it to the known distribu-
tion of various galactic foregrounds. Spider will map the cleanest area of the microwave sky, with a sky coverage
much larger than that of many comparable instruments.
4. FOREGROUNDS AND SYSTEMATICS
Spider is designed to limit the effect of galactic and atmospheric foregrounds upon the instrumental perfor-
mance. The locations and widths of the Spider bands are chosen to avoid prominent atmospheric spectral
lines; in combination with the stratospheric vantage point provided by a balloon flight, this greatly reduces the
atmospheric contributions of noise and excess loading. Spider’s 90 and 150 GHz bands target the frequencies
where the CMB is brightest in comparison to galactic foregrounds, and are further optimized to avoiding the
galactic CO line. The 280 GHz band will map the polarized foreground emission of galactic dust; in combination
with Planck maps of dust emission intensity, this will allow us to subtract any contribution from polarized dust
emission with high accuracy.
Instrumental systematic effects present a huge challenge for the measurement of nanoKelvin polarization
signals on the sky. MacTavish et al.9have investigated the instrumental systematics of Spider using a simulation
of the full data analysis pipeline. This set of simulations determined a set of specifications on instrumental design
and on in-flight or pre-flight knowledge of various instrumental parameters. These initial simulations were focused
upon a flight of Spider from Alice Springs, Australia, with greater sky coverage and a spinning-gondola scan
strategy; detailed simulations of an Antarctic flight are still in progress.
Figure 3. Upper left: The sky coverage for the Antarctic LDB flight. The integration time per pixel, for a single column
of a Spider array, is shown in celestial coordinates. Contours of galactic latitude are drawn for reference at b = (0,−20).
Only a single column is shown to make the pattern of cross linking more evident. The coverage of the full array will be
smoothed in ∼RA by the ∼8◦field of view. Spider will cover about 8% of the full sky, including the majority of the area
in the Southern hemisphere that is not heavily contaminated by Galactic emission. The rectangular outline indicates the
region of sky easily scanned from the geographic South Pole with low atmospheric loading and galactic foregrounds.5The
large oval shows the CMB field observed by BOOMERanG,21,22while the smaller oval shows the EBEX field.23By virtue
of its small, easily-shielded apertures, Spider can scan much closer to the sun (lower in RA) than BOOMERanG, and
therefore cover more sky. Upper right: The seven year WMAP K-band data, a tracer of Galactic synchrotron emission.24
The bright point sources are mostly quasars at redshift z ∼ 0.5 that will be used in Spider’s pointing reconstruction.
Lower left: The seven year WMAP W-band data. The 90 GHz data are near the minimum of the total intensity of the
Galactic foregrounds over much of the sky. Lower right: The IRAS 100 µm map, showing the morphology of the thermal
emission of Galactic dust.25,26
5. SPIDER PAYLOAD
The Spider payload, shown in Figure 4, consists of six monochromatic refracting telescopes housed within a
single liquid helium cryostat. The gondola frame is derived from the successful BLAST27design. The frame is
constructed from carbon fiber tubes in order to maintain great strength at very low mass, allowing it to support
a payload mass of ∼2000 kg under launch accelerations while itself weighing only ∼110 kg. An azimuth reaction
wheel allows the payload to operate in two major observing modes: back-and-forth scanning in azimuth or full
azimuthal rotation; the former is most appropriate for daytime observation, the latter for operation at night.
The elevation of the inner frame is adjustable with a simple linear actuator similar to the BOOMERanG design.
The pointing and pointing reconstruction systems build on experience from the BOOMERanG28and BLAST
designs. Pointing information is provided by two tracking star cameras, rate gyroscopes, differential GPS, and
a sun sensor. Extensive sun shielding and baffling, combined with the relatively small optical apertures of the
Spider telescopes, allows the instrument to scan closer to the sun for increased sky coverage.
The cryostat for the Spider instrument uses liquid helium-4 (LHe) to cool the instrument during its flight. All six
telescope inserts and a ∼1000 liter LHe tank are contained in a single outer vacuum vessel fabricated by Redstone
Figure 4. An illustration of the Spider payload, showing the liquid helium cryostat and the surrounding carbon-fiber
frame. The bearing atop the frame allows the cryostat to scan in azimuth, while a linear actuator adjusts the bore sight
elevation. A sun shield protects the cryostat from solar heating. The solar panels and electronics packages are not shown.
Aerospace. The primary LHe tank is maintained at 108 kPa (∼1 atm) and has an expected minimum hold time
of 25 days. A smaller (∼20 liter) superfluid LHe tank is continuously fed from the main tank through a capillary
and controlled at a vapor pressure near 100 Pa to provide cooling power at ∼1.5 K. Each focal plane is further
cooled to 260 mK by its own closed-cycle3He sorption refrigerator. These sub-Kelvin coolers are recycled every
48-72 hours. Further details of Spider’s thermal architecture are described elsewhere in these proceedings.11
5.3 Optical design
The optical design of Spider is based on that of the successful Robinson/Bicep telescope.29,30Each telescope
is a monochromatic, telecentric refractor containing anti-reflection-coated polyethylene lenses cooled to 4 K.
The aperture field distribution of the primary is smoothly tapered with a 4 K Lyot stop to reduce detector
background. The beam of each pixel subtends 35 arc minutes (FWHM) on the sky. The Spider telescope design
is described further in a separate contribution to these proceedings.31
A half-wave plate is mounted to the aperture of each telescope and cooled to 4 K. The wave plate assembly
consists of a single birefringent sapphire plate coated with a single layer of fused quartz on each side. This
assembly may be rotated in flight using a worm gear drive train, thus rotating the angle of polarization sensitivity
on the sky while leaving the beams unchanged. This allows a full measurement of the sky polarization using each
individual detector, eliminating or reducing many potential systematic effects (e.g. gain or pointing mismatches
within a detector pair). Spider’s single-frequency telescopes simplify the wave plate design and implementation.
The optical performance of a prototype Spider wave plate assembly is described elsewhere in these proceedings.10
The Spider optical system is constructed to take full advantage of the very low atmospheric background
available at balloon altitudes by minimizing the stray light incident upon the detectors. As described above,
the principal optical elements - lenses, Lyot stop, and half-wave plate - are cooled to 4 K to reduce internal
thermal radiation. Detector beam sidelobes within the telescope tube terminate on an inner sleeve cooled to 2
K. The focal plane is protected from out-of-band radiation by an extensive cooled filter stack containing infrared
shaders, hot-pressed mesh filters, and a nylon filter. In flight the Spider aperture will be covered by a thin-film
polymer window with low emissivity; a thicker retractable HDPE window will be employed to withstand the
greater atmospheric pressure on the ground.
Figure 5. Left: A partially assembled 150 GHz Spider test focal plane, with three of four detector tile slots filled.
The detector tiles each contain 64 spatial pixels and 128 TES bolometers. The 16 SQUID multiplexer chips and their
associated Nyquist inductor chips are encapsulated in four magnetically-shielded boxes behind the focal plane, connected
to the detectors by flexible superconducting circuits visible to the right and left of the tiles; in this image the flexible
circuits are covered by protective Al boxes which are not present in the final configuration. The tiles are held in place by
metal clips that maintain pressure despite thermal contraction. Top right: Closer view of a spatial pixel, showing phased
array of slot antennas feeding two TESs at bottom. Bottom right: Close-up of a single TES assembly, showing the TES
island and the SiN thermal isolation legs. The meandered leg design allows for low thermal conductance in a narrow
6. FOCAL PLANE
6.1 Focal plane
The focal plane architecture of each Spider refractor is derived from that of the Bicep 2 instrument, with
extensive modifications to improve magnetic shielding.12
plane unit. Four Si bolometer arrays constitute the microwave-sensitive elements of each focal plane. These
detector tiles are supported at a distance of 1/4-wavelength above a superconducting Nb backshort plate, which
defines an integrating cavity and provides magnetic shielding. Flexible superconducting circuits connect the
arrays to their associated SQUID amplifiers, which are housed within a magnetically-shielded box behind the
focal plane. The entire assembly is cooled to ∼300 mK by the3He refrigerator. The temperatures of each tile
and of the copper support plate are read out using neutron-transmutation-doped (NTD) Ge thermistors.
Figure 5 shows a partially-assembled Spider focal
6.2 Bolometer arrays
Each Spider refractor focuses light onto four large-format arrays of antenna-coupled bolometers,32pictured in
Figure 5. These arrays integrate beam and band defining elements with polarization-sensitive detectors into a
single monolithic package, without a need for external feed horns. Each array is a Si tile photolithographically
patterned with an 8×8 array of spatial pixels (6×6 for 90 GHz arrays) with ∼2Fλ spacing. A spatial pixel
consists of two interleaved arrays of slot antennas, one each for the two perpendicular polarization components
of incident light. A summing tree of microstrip transmission lines link each array of slots to form a single
antenna. The slots are summed in-phase with one another, producing a diffraction-limited beam that couples to
the optics with single-moded throughput. This arrangement gives each pixel a ∼13◦FWHM beam, with a ∼25%
bandwidth (set by the slot dimensions) and a first sidelobe at -15 dB. The output of each tree passes through
an on-chip band-defining filter and terminates on a superconducting transition-edge sensor (TES) bolometer.33
Systematic differences between the two polarization channels in each spatial pixel are limited by their shared
optical path, the physical proximity of their bolometers, and their shared readout electronics chain.
The Spider bolometers are similar in design to those used in Bicep 2,34but have been optimized for the
far lower optical background available at a suborbital platform. The TES is a thin film of Ti (Tc≈ 500 mK) on
a silicon nitride membrane, thermally isolated from the tile substrate by narrow legs of silicon nitride. Power
(145 GHz optics)
(145 GHz optics)
Mean optical efficiency
Figure 6. Left: Mean end-to-end frequency response of Spider 150 GHz and 96 GHz test detectors, measured through
science-grade 150 GHz optics. Note that the 96 GHz detector bands are distorted by the mismatched optics, introducing
ripples in the passband and truncating the response before the upper band edge. The band center of the science-grade
detectors will be shifted from 96 GHz to ∼90 GHz to avoid background from O and CO lines. Right: Near-field beam
map of a 150 GHz Spider detector, measured at the cryostat aperture through science-grade optics.
28067 17(2×) 256
Table 1. Spider observing bands, pixel and detector counts, and single-detector and instrument sensitivities. The latter
are quoted by dividing the single-detector sensitivity by√Ndet, assuming a detector yield of 85%. The quoted sensitivities
at 90 and 150 GHz are typical of measurements made under flight-like loading conditions; the performance of the 280 GHz
devices has not yet been measured under a representative load. Sensitivities in parentheses are quoted in Rayleigh-Jeans
units appropriate for dust emission.
received by the antenna is dissipated in a Au termination resistor on the island, which is maintained at the
TES critical temperature by electrothermal feedback. The Spider TES islands are designed to have somewhat
lower island heat capacities and much lower thermal conductances to the tile than those used by Bicep 2, as
appropriate to the ∼5× lower background at float altitude. The 150 GHz Spider detectors use a meandered
leg design to achieve an extremely low thermal conductance (G=20 pW/K for a 150 GHz sensor) within a
narrow geometry, the latter chosen to limit direct coupling of incident microwaves to the membrane. These low
conductances give the Spider arrays very low noise levels (see Table 1), but at the cost of relatively low TES
saturation powers. For beam characterization under laboratory loading conditions we make use of a secondary
Al TES with much higher saturation power that is connected in series with the Ti TES.
Figure 6 shows results from optical characterizations of full detector arrays in the Spider test cryostat.
All measurements were taken in a 150 GHz Spider telescope, with a full set of optics appropriate for this
frequency. Optical efficiencies, band widths, and noise performance meet requirements for deployment. We
have not yet carried out a full characterization of the far-field response of the Spider beams, but results from
preliminary laboratory tests and from measurements of the BICEP2 instrument in the field30indicate that the
arrays perform adequately for Spider’s needs. The Spider, Bicep 2, and Keck collaborations continue to
collaborate on improving the designs of these arrays. Table 1 lists the baseline frequency coverage and expected
sensitivity of the full Spider instrument.
6.3 Readout system
The hundreds of TESs making up each Spider focal plane are read out using a time-domain SQUID multiplexer
system developed by NIST.35The changing current through each TES is detected by a corresponding first-stage
SQUID. These SQUIDs are switched on one at a time in rapid succession, so that each group of 33 SQUID
channels (32 connected to bolometers plus one “dark” channel to monitor amplifier drifts) may be read out
through a single set of wires to room temperature. The output of each group of first-stage SQUIDs is amplified
by a second-stage SQUID and a series SQUID array36before reaching an ambient-temperature amplifier. This
arrangement greatly reduces the number of wires necessary to instrument these large-scale focal planes. To
maximize the effectiveness of pair-differencing in rejecting amplifier noise, the two polarizations of each spatial
pixel are read out through adjacent first-stage SQUIDs in a common amplifier chain.
The TESs and SQUID multiplexer system are controlled and read out using the multi-channel electronics
(MCE),37an ambient-temperature electronics crate initially designed for the SCUBA-2 instrument.38A single
MCE crate maintains each focal plane, providing all necessary current and flux biases and linearizing the response
of each SQUID channel using a digital feedback loop. All communication with the gondola computers is through
optical fiber. A single crystal clock at 50 MHz synchronizes the timing of all six MCE crates on the gondola.
The MCE is highly programmable, allowing for flexible scripting and reconfiguration of science data acquisition
and regular bolometer characterization. In standard operation each TES is revisited every ∼66µs and data are
recorded to solid-state disk at ∼400 Hz; other data acquisition modes are available for system characterization.
6.4 Magnetic shielding
By its nature, the Spider readout system is sensitive to the influence of external magnetic fields. Each of the
SQUIDs in the amplifier chain is a sensitive magnetometer, affected by tiny changes in the flux linking the SQUID
loop. The TESs themselves are also magnetically sensitive through the dependence of the superconducting film’s
critical temperature on magnetic field. Each SQUID on the focal plane is wound as a second-degree gradiometer
to reduce the influence of external fields, but changes in the focal plane’s magnetic environment can nonetheless
mimic sky signals. Of particular concern is the motion of the gondola through the Earth’s magnetic field, which
could induce a scan-synchronous signal fixed in a terrestrial (rather than celestial or instrumental) coordinate
system, corrupting low-? modes of the map. Magnetic shielding is thus a critical requirement for the Spider
The Spider telescope and focal plane are designed to shield the detectors and SQUIDs from external magnetic
fields. The Spider shield design incorporates several improvements upon the configuration used for BICEP2,
developed with the aid of COMSOL simulations and extensive laboratory measurements. Layers of high-µ
material line each telescope tube and surround each focal plane assembly. The Nb backshort further excludes
magnetic fields from the vicinity of the focal plane. The SQUID chips are further protected within a low-
field enclosure behind the focal plane, encased inside several additional layers of high-µ and superconducting
material. No ferromagnetic materials were used in the construction of the telescope inserts or LHe cryostat.
Spider’s magnetic shielding is described in greater detail elsewhere in these proceedings.12
Spider is unique as a powerful sub-orbital millimeter-wave polarimeter that can observe a large fraction of
the sky. By combining the massive mapping speed provided by large-format multiplexed TES arrays with an
optical design optimized for polarimetry, it has the power needed to map the polarization of the CMB with
unprecedented fidelity. It’s initial Antarctic flight will measure or powerfully constrain the B-mode signal from
primordial gravitational waves, as well as making measurements of polarized foregrounds and of the lensing
contribution to the CMB B-mode with lasting value.
Spider will also serve as a crucial pathfinder to test new technologies for EPIC/CMBpol, a proposed satellite
mission to make definitive maps of the polarization of the millimeter-wave sky.39The large-format detector
array technology deployed in Spider is an ideal candidate for a space mission, allowing the rapid construction
of kilopixel focal planes without the need for external feedhorn and filter hardware. Following in the tradition of
BOOMERanG and BLAST, Spider will test these technologies under conditions directly applicable to a space
mission: low optical background, a limited power budget, tight mass constraints, and autonomous operation.
The Spider collaboration gratefully acknowledges the support of NASA (grant number NNX07AL64G), the
Gordon and Betty Moore Foundation, and NSERC. WCJ acknowledges the support of the Alfred P. Sloan
Foundation. JPF is partially supported by a Moore Postdoctoral Fellowship in Experimental Physics.
The Spider collaboration also extends special gratitude to Andrew E. Lange, who passed away on January
22. Andrew was a leading light of the cosmology community and a driving force behind the Spider project. He
is greatly missed by his many collaborators, past and present.
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