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{{Short description|Balloon-borne astronomical experiment}}
'''Spider''' is a balloon-borne experiment designed to search for [[cosmic gravitational wave background|primordial gravity waves]] imprinted on the [[cosmic microwave background]] (CMB). Measuring the strength of this signal puts limits on [[Inflation (cosmology)|inflationary theory]].▼
{{Infobox telescope}}
▲'''Spider''' is a balloon-borne experiment designed to search for [[cosmic gravitational wave background|primordial
[[File:Hang test pano.jpg|thumb|alt=Spider on the launch vehicle|The Spider experiment hanging from the launch vehicle prior to its first flight over Antarctica.]]
The Spider instrument consists of six degree-resolution telescopes cooled to liquid Helium temperature (4 [[Kelvin|K]]) which observe at frequencies of 100 GHz, 150 GHz, and 280 GHz (corresponding to wavelengths of 3 mm, 2 mm, and 1.1 mm). Each telescope is coupled to a [[polarization (waves)|polarisation]]-sensitive [[transition edge sensor|transition-edge bolometer]] (TES) array cooled to 300 [[Kelvin|mK]]. Spider was the first instrument to successfully demonstrate time-domain multiplexed TES detectors in a space-like environment. At the time of the first flight over Antarctica in 2015, Spider was the most sensitive microwave instrument ever made.<ref>{{cite book |arxiv=2012.12407 |doi=10.1117/12.2562941 |chapter=Design and pre-flight performance of SPIDER 280 GHZ receivers |title=Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X |year=2020 |last1=Shaw |first1=E. C. |last2=Ade |first2=P.A.R. |last3=Akers |first3=S. |last4=Amiri |first4=M. |last5=Austermann |first5=Jason E. |last6=Beall |first6=James A. |last7=Becker |first7=D.T. |last8=Benton |first8=S.J. |last9=Bergman |first9=A. S. |last10=Bock |first10=J.J. |last11=Bond |first11=J.R. |last12=Bryan |first12=S.A. |last13=Chiang |first13=H.C. |last14=Contaldi |first14=C.R. |last15=Domagalski |first15=R.S. |last16=Dore |first16=O. |last17=Duff |first17=S. M. |last18=Duivenvoorden |first18=A.J. |last19=Eriksen |first19=H.K. |last20=Farhang |first20=M. |last21=Filippini |first21=J. P. |last22=Fissel |first22=L.M. |last23=Fraisse |first23=A.A. |last24=Freese |first24=K. |last25=Galloway |first25=M. |last26=Gambrel |first26=A. E. |last27=Gandilo |first27=N.N. |last28=Ganga |first28=K. |last29=Grigorian |first29=A. |last30=Gualtieri |first30=R. |page=173 |isbn=9781510636934 |s2cid=229363672 |editor-first1=Jonas |editor-first2=Jian-Rong |editor-last1=Zmuidzinas |editor-last2=Gao |display-authors=1 }}</ref><ref>{{Cite arXiv| eprint=2103.13334 | last1=Collaboration | first1=SPIDER | last2=Ade | first2=P. A. R. | last3=Amiri | first3=M. | last4=Benton | first4=S. J. | last5=Bergman | first5=A. S. | last6=Bihary | first6=R. | last7=Bock | first7=J. J. | last8=Bond | first8=J. R. | last9=Bonetti | first9=J. A. | last10=Bryan | first10=S. A. | last11=Chiang | first11=H. C. | last12=Contaldi | first12=C. R. | last13=Doré | first13=O. | last14=Duivenvoorden | first14=A. J. | last15=Eriksen | first15=H. K. | last16=Farhang | first16=M. | last17=Filippini | first17=J. P. | last18=Fraisse | first18=A. A. | last19=Freese | first19=K. | last20=Galloway | first20=M. | last21=Gambrel | first21=A. E. | last22=Gandilo | first22=N. N. | last23=Ganga | first23=K. | last24=Gualtieri | first24=R. | last25=Gudmundsson | first25=J. E. | last26=Halpern | first26=M. | last27=Hartley | first27=J. | last28=Hasselfield | first28=M. | last29=Hilton | first29=G. | last30=Holmes | first30=W. | title=A Constraint on Primordial $B$-Modes from the First Flight of the SPIDER Balloon-Borne Telescope | year=2021 | class=astro-ph.CO | display-authors=1 }}</ref>
The primary science goals include:
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# searching for the signature of inflationary gravitational waves in the CMB polarization
# characterization of the polarization properties of the emission from our own Milky Way Galaxy
The first balloon flight of the experiment launched in January 2015 from [[McMurdo Station]], Antarctica, with support from NASA's [[Columbia Scientific Balloon Facility]]. This Long Duration Balloon flight lasted for about 17 days, mapping about 10% of the full sky. The data from this flight produced high signal-to-noise images of the intensity and linear polarization of the Cosmic Microwave Background, with noise levels 3—5 times lower than the [[Planck spacecraft]] in the same region of the sky, resulting in precise measurements of the CMB and Galactic foreground radiation, as well as a robust limit on the cosmological tensor-to-scalar ratio. Further flights planned for successive seasons enable upgrades and changes to the modular telescope, increased frequency coverage and depth.
==References==
{{Reflist}}
==External links==
* [
* [https://spider.princeton.edu/ Spider Homepage]
* [http://spider.princeton.edu Spider 2014/15 campaign blog]
* [https://arxiv.org/abs/2103.13334 The Spider Collaboration, "A Constraint on Primordial B-Modes from the First Flight of the SPIDER Balloon-Borne Telescope"]
{{CMB experiments}}
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[[Category:Balloon-borne telescopes]]
[[Category:Cosmic microwave background experiments]]
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