Design and calibration of the 34 GHz Yale microwave cavity experiment

Slocum, P. L.; Baker, O. K.; Hirshfield, J. L.; Jiang, Yong; Malagon, Ana; Martín, A.; Shchelkunov, Sergey V.; Szymkowiak, Andrew E.

doi:10.1016/j.nima.2014.10.013

Cited by 7 publications

(7 citation statements)

References 44 publications

(63 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…where Y is the measured ratio of hot/cold noise power spectra and A is the measured hot/cold gain ratio. 15 N A should be independent of the presence of the cavity mode in the spectrum, and empirically it also exhibits no systematic dependence on RF frequency. Thus we can break the degeneracy in Y -factor measurements around the TM 010 resonance by subtracting ( NA ) j , the average receiver added noise obtained from off-resonance Y -factor measurements.…”

Section: A the Rescaling Proceduresmentioning

confidence: 95%

“…which did not however adopt our frequency-domain approach or consider the effects of filter-induced correlations. See Ref [15]. for further discussion of this experiment 9.…”

mentioning

confidence: 99%

“…Technically, N T is a function of frequency evaluated at ν ci , but it changes negligibly over our tuning range, so we suppress its idependence. j-dependence due to the finite width of the analysis band is of course much smaller still 15. The additional factors multiplying the Ncav term account for the fact that it contributes only to the cold load noise measurement, whereas N A contributes to the noise in both the hot load and the cold load; see also discussion in Ref [6]…”

mentioning

confidence: 99%

See 2 more Smart Citations

HAYSTAC axion search analysis procedure

et al. 2017

View full text Add to dashboard Cite

We describe in detail the analysis procedure used to derive the first limits from the Haloscope at Yale Sensitive to Axion CDM (HAYSTAC), a microwave cavity search for cold dark matter (CDM) axions with masses above 20 µeV. We have introduced several significant innovations to the axion search analysis pioneered by the Axion Dark Matter eXperiment (ADMX), including optimal filtering of the individual power spectra that constitute the axion search dataset and a consistent maximum likelihood procedure for combining and rebinning these spectra. These innovations enable us to obtain the axion-photon coupling |gγ| excluded at any desired confidence level directly from the statistics of the combined data.

show abstract

Section: A the Rescaling Proceduresmentioning

confidence: 95%

“…which did not however adopt our frequency-domain approach or consider the effects of filter-induced correlations. See Ref [15]. for further discussion of this experiment 9.…”

mentioning

confidence: 99%

mentioning

confidence: 99%

See 1 more Smart Citation

HAYSTAC axion search analysis procedure

et al. 2017

View full text Add to dashboard Cite

show abstract

“…ADMX is suited to masses < 10 µeV and has currently set constraints between 1.9 µeV < m a < 3.69 µeV [21,46]. Larger masses require adjustments to the cavity and amplification technology [96,97]. The Yale Wright Laboratory experiment of Refs.…”

Section: Discussionmentioning

confidence: 99%

Axion astronomy with microwave cavity experiments

O’Hare

Green

2017

Phys. Rev. D

View full text Add to dashboard Cite

Terrestrial searches for the conversion of dark matter axions or axion-like particles into photons inside magnetic fields are sensitive to the phase space structure of the local Milky Way halo. We simulate signals in a hypothetical future experiment based on the Axion Dark Matter eXperiment (ADMX) that could be performed once the axion has been detected and a frequency range containing the axion mass has been identified. We develop a statistical analysis to extract astrophysical parameters, such as the halo velocity dispersion and laboratory velocity, from such data and find that with only a few days integration time a level of precision can be reached matching that of astronomical observations. For longer experiments lasting up to a year in duration we find that exploiting the modulation of the power spectrum in time allows accurate measurements of the Solar peculiar velocity with an accuracy that would improve upon astronomical observations. We also simulate signals based on results from N-body simulations and find that finer substructure in the form of tidal streams would show up prominently in future data, even if only a subdominant contribution to the local dark matter distribution. In these cases it would be possible to reconstruct all the properties of a dark matter stream using the time and frequency dependence of the signal. Finally we consider the detection prospects for a network of streams from tidally disrupted axion miniclusters. These features appear much more prominently in the resolved spectrum than suggested by calculations based on a scan over a range of resonant frequencies, making the detection of axion minicluster streams more viable than previously thought. These results confirm that haloscope experiments in a post-discovery era are able to perform "axion astronomy".

show abstract

“…Such experiments require less assumptions about the nature of these WISP particles (they do not require the particles to constitute halo dark matter), but are inherently less sensitive as they require two WISP-photon conversions. Several microwave haloscope [23][24][25][26][27][28] and LSW [29][30][31][32][33] experiments have been conducted to date, with no reports of any signals congruent with WISP detection. The majority of these searches have been conducted below 10 GHz due to a multitude of technical issues and limitations.…”

Section: Introductionmentioning

confidence: 99%

Cross-Correlation Signal Processing for Axion and WISP Dark Matter Searches

McAllister

Parker

Ivanov

et al. 2019

IEEE Trans. Ultrason., Ferroelect., Freq. Contr.

View full text Add to dashboard Cite

The search for dark matter is of fundamental importance to our understanding of the universe. Weakly-Interacting Slim Particles (WISPs) such as axions and hidden sector photons (HSPs) are well motivated candidates for the dark matter. Some of the most sensitive and mature experiments to detect WISPs rely on microwave cavities, and the detection of weak photon signals. It is often suggested to power combine multiple cavities, which creates a host of technical concerns. We outline a scheme based on cross-correlation for effectively power combining cavities and increasing the signal-to-noise ratio of a candidate WISP signal.

show abstract

Design and calibration of the 34 GHz Yale microwave cavity experiment

Cited by 7 publications

References 44 publications

HAYSTAC axion search analysis procedure

HAYSTAC axion search analysis procedure

Axion astronomy with microwave cavity experiments

Cross-Correlation Signal Processing for Axion and WISP Dark Matter Searches

Contact Info

Product

Resources

About