Dark Matter – Direct Detection| Dark Matter – Direct Detection |
In General, Timeline
> s.a. cosmic rays [positron excess]; dark-matter distribution.
* 1996: High-energy-style
experiments have been running for years, in particular looking for axions.
* 2000: Evidence for WIMPS
reported by the DAMA collaboration at the INFN Gran Sasso Lab, based on seasonal
variation of events in a shielded NaI scintillator supposedly detecting 50
mp particles – controversial,
and contradicted by the more sophisticated Stanford University CDMS team of B Cabrera.
* 2005: DAMA results still
controversial, but still quoted.
* 2008: New DAMA claims of
yearly detector-signal modulation, indicating a dark matter "wind";
CoGeNT disputes WIMPS as source.
* 2009: CDMS events signal possible
direct detection of dark matter, but need to be confirmed by more statistics.
* 2011: CoGeNT findings support
dark-matter detection by the DAMA/LIBRA detector [@ news
pw(11)jun].
* 2013: Alpha Magnetic Spectrometer (AMS)
collaboration reports an excess of positrons in the cosmic-ray flux; LUX collaboration
reports stringent upper limits on the cross section of WIMP-nucleon elastic scattering.
* 2014: CoGeNT data confirm the annual
modulation of events seen by DAMA; Three experiments will get upgrades (SuperCDMS and
LUX-ZEPLIN search for WIMPS, ADMX-Gen2 search for axions); DAMA signal may be due to
neutrons created by solar neutrinos and atmospheric muons.
* 2016: In the current experiment,
DAMA/LIBRA pegs the statistical significance of the detected annual modulation at 9.3
standard deviations.
* 2017: The upgraded XENON1T experiment
in Gran Sasso and PandaX-II in Japan report no signals; Feld "in a state of major
disruption".
* 2018: COSINE-100, using the same type
of detector as DAMA, reports no signs of dark matter.
* 2021: ANAIS Collaboration also reports no sign of WIMPS.
@ Reviews: Cline SA(03)mar;
Bertone a0710-talk;
Hooper & Baltz ARNPS(08)-a0802;
Feng AIP(09)-a0908;
Armengaud a1003-ln;
Rau PPN(11)-a1103-proc;
Porter et al ARAA(11);
Baudis PDU(12)-a1211 [the next decade];
Bauer et al PDU(15)-a1305-rp,
Arrenberg et al a1310-rp [approaches to detection];
Queiroz a1605-conf.
@ Status: news NYT(08)apr,
pw(08)apr,
pw(08)aug
[disputed claims of WIMP detection at DAMA];
news sn(09)dec,
pw(09)dec,
NYT(09)dec [rumors of WIMP detection at CDMS];
news NYT(10)may [XENON100];
news SA(14)jul [2nd generation searches];
news guard(16)feb [current efforts];
news pt(16)jul
[SABRE experiment built to directly check DAMA results];
Hooper Phy(17)jan
[no signal from XENON1-T and PandaX-II data];
COSINE-100 Collaboration Nat(18)dec
+ news sn(18)dec,
pt(18)dec [no signal];
Amare et ANAIS a2103
+ news sn(21)mar [no signal].
Experiments on Earth
> s.a. fine structure constant variations.
* WIMP detection: Detectors are usually large
and underground; They aim to see the results of collisions between WIMPS and atomic nuclei.
* Annual modulation: Were it not for the Sun's
gravity, the signal would be expected to peak around June 1, when the Earth is moving against the
direction of the dark matter wind; The effect of the Sun should shift the seasonal peak earlier
by three months or so.
@ Reviews: Smith & Lewin PRP(90);
Sumner LRR(02);
Loidl ap/02-proc;
Baudis IJMPA(06)ap/05-in;
Cooley ap/06-proc;
Baudis a0711-proc;
Fornengo ASR(08)ap/06-conf;
Schnee in(10)-a1101-ln;
Marrodán & Rauch JPG(16)-a1509;
Spooner JPSJ(17)-a0705;
Liu et al nPhys(17)-a1709.
@ Experimental searches:
Pretzl ed-NJP(00) [focus issue];
Araújo pw(05)may;
Beck JPCS(06)ap/05 [using Josephson junctions];
Saab MPLA(08);
Kane & Watson MPLA(08)-a0807 [and the LHC];
Gelmini IJMPA(08);
Freese a0812-proc;
Lang & Seidel NJP(09)-a0906 [CRESST];
Estrada JPCS(10)-a0911 [using CCDs];
Irastorza a0911-proc [in underground laboratories];
Sandick ASP-a1001;
Bertone et al PRD(10)-a1005 [combining LHC and direct detection data];
Censier a1110-proc [non-directional];
Arina et al JCAP(11) [Bayesian view];
Pato JCAP(11);
Aguilar et al PRL(13)
+ Coutu Phy(13)
+ news NYT(13)apr [positron excess in cosmic rays];
Lee et al PRL(14)
+ news sa(14)jan [annual modulation];
Aad et ATLAS Collaboration PRL(14) [constraints on masses and interactions];
Askew et al IJMPA(14) [at hadron colliders];
Sorensen PRD(15)-a1412 [modeling and sensitivity of direct-detection experiments];
Bernabei IJMPD(16);
news pt(19)mar
[future FASER (Forward Search Experiment) at CERN to search for dark photons];
> s.a. Nightmare Scenario.
@ WIMPS at DAMA:
Bernabei et al RNC(03)ap;
Aalseth et al PRL(08) [modulation];
Davis PRL(14) [DAMA signal and neutrons].
@ Other WIMP detectors:
Morales NPPS(00)ap/99;
Beg et al APL(02)
+ pn(02)apr;
Luscher ap/03 [Boulby mine];
Morgan CP(03),
Seidel ap/03-proc [rev];
Birkedal et al PRD(04)hp [at colliders];
Freese et al PRL(04) [Sagittarius Stream];
Chardin ap/04-in [status];
Mirabolfathi ap/04-conf;
news sr(06)nov [CDMS II experiment];
Landsman ap/06-proc [IceCube as dark matter detector];
Schnee AIP(07)ap/06 [rev];
Benetti et al APP(08)ap/07 [liquid Ar in Gran Sasso];
Wai for GLAST AIP(07)ap;
Behnke et al Nat(08)-a0804 [limits from bubble chamber experiment];
Sciolla et al a0810-proc [DMTPC];
Ahmed et CDMS PRL(09)
+ van Bibber Phy(09) [limits on interactions];
Sciolla MPLA(09),
Billard et al a1004-proc [directional];
Schnee Phy(10) [XENON100 detector];
news nat(11)apr [bounds on WIMPs and supersymmetry];
Cline MPLA(11);
Green MPLA(12)-a1112 [astrophysical uncertainties];
Mayet et al proc(13)-a1207 [directional detection];
LUX Collaboration PRL(14)-a1310,
news S&T(13)nov,
Sanders a1311 [doubts on WIMP detection claims];
Lang Phy(13) [conficting results];
Bernabei et al EPJC(14)-a1403 [no diurnal modulation seen];
Cline a1406 [rev];
Billard PRL(15) [strategies for identifying WIMPs];
XENON Collaboration PRL(17)
+ Hoper Phys(17) [no evidence, limits].
@ Other proposals: Goodman et al PRD(10)-a1008 [constraints from colliders];
Livio & Silk Nat(14)mar-a1404 [broadening the search];
Ruppin et al PRD(14) [discriminating dark matter from neutrinos];
Cherry et al PRL(15)-a1501 [detecting annihilation products];
Graham et al PRD(16)-a1512 [using accelerometers];
Levy et al JINST(16)-a1601 [xenon bubble chamber];
Hochberg et al PRL(16) [superconducting detectors];
Schutz & Zurek PRL(16) [with superfluid He];
Arvanitaki et al PRX(18) [resonant absorption in molecules];
Carney et al PRD-a1903 [using only the gravitational coupling];
Calmet a1907 [with quantum sensors];
Sidhu et al a1907 [the human body as a dark matter detector].
@ Supersymmetric-dark-matter search: Vergados AIP(02)ap;
Cline ap/03-conf;
Ellis et al PRD(05)hp.
@ Search for other particles:
news pw(14)oct [hidden photons];
Batell et al PRL(14),
Aprile et al PRL(19)
[limits on the dark photon from other experiments].
> Online resources:
DAMA site;
CoGeNT site.
Other Direct Observation > s.a. tests of general relativity
[cosmological]; dark-matter distribution [evidence from solar or galactic scales].
* Microlensing: Amount produced by small stars
in some galaxies indicates 8–16 times as much mass as from visible stars [@ Langston et al
Nat(90)mar];
There may be more stars in halos and gray dwarves in disks than we thought.
@ Detectors in space: Feng NPPS(04);
Réfrégier et al SPIE(06)ap [DUNE proposed mission];
Kusenko IJMPD(08)ap/06-proc [sterile neutrinos];
Strigari et al ApJL(07)ap [astrometry with SIM PlanetQuest];
Roberts et al nComm(17)
+ news cosmos(17)oct [GPS satellites];
Bertoldi et al a1908 [AEDGE, using cold atoms].
@ MACHOS / microlensing:
Bennett et al ASP-ap/95;
Gould ap/96-conf;
De Paolis et al ap/97-MG8,
ap/97-MG8;
Sutherland RMP(99)ap/98;
Jetzer AIP(99)ap/98;
Alcock et al ApJL(01)ap/00;
Lasserre et al A&A-ap/00.
@ Other lensing: Massey et al RPP(10)-a1001 [in general];
Huterer GRG(10)-a1001 [weak];
Hsueh et al MNRAS(16)-a1601 [bias in observational measurements];
Mishra-Sharma et al PRL(20) [weak lensing].
@ Related topics:
Sikivie & Wick PRD(02) [solar wakes];
Bourjaily EPJC(05)ap/04-conf [determining the local density];
Gu et al hp/05 [and dark energy effects];
Clowe et al ApJL(06)ap
+ sr(06)aug,
Clowe & Zaritsky pw(07)feb [galaxy cluster collision];
Clarke & Foot a1512 [plasma].
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send feedback and suggestions to bombelli at olemiss.edu – modified 25 mar 2021