AEDGE: Atomic Experiment for Dark Matter and Gravity Exploration in Space
- El-Neaj, Yousef Abou et al
- arXiv:1908.00802KCL-PH-TH/2019-65CERN-TH-2019-126
| \it Comparison of the strain measurements possible with AEDGE and other experiments, showing their sensitivities to BH mergers of differing total masses at various redshifts $z$, indicating also the time remaining before the merger. The solid lines correspond to equal mass binaries and the dashed ones to binaries with very different masses, namely $3000M_\odot$ and $30M_\odot$. Also shown is the possible gravitational gradient noise (GGN) level for a km-scale terrestrial detector, which would need to be mitigated for its potential to be realized. This figure illustrates the potential for synergies between AEDGE and detectors observing other stages of BH infall and merger histories. |
| \it Left panel: Examples of GW spectra from cosmic strings with differing tensions $G\mu$. The dashed lines show the impact of the variation in the number of SM degrees of freedom. Right panel: Detail of the effect on the GW spectrum for the case $G \mu = 10^{-11}$ of a new particle threshold at various energies $T_\Delta \ge 100$\,MeV with an increase $\Delta g_* = 100$ in the number of relativistic degrees of freedom. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to linear scalar DM interactions with electrons (top), photons (middle) and via the Higgs portal (bottom), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza, Hees:2016gop}. |
| \it Left panel: Examples of GW spectra from cosmic strings with differing tensions $G\mu$. The dashed lines show the impact of the variation in the number of SM degrees of freedom. Right panel: Detail of the effect on the GW spectrum for the case $G \mu = 10^{-11}$ of a new particle threshold at various energies $T_\Delta \ge 100$\,MeV with an increase $\Delta g_* = 100$ in the number of relativistic degrees of freedom. |
| \it Left panel: Example of the GW spectrum in a classical scale-invariant extension of the SM with a massive $Z^\prime$ boson, compared with various experimental sensitivities. The dashed line shows the contribution to the spectrum sourced by bubble collisions, the dot-dashed line shows the contribution from sound waves, and the dotted line shows the contribution from turbulence. Right panel: Examples of spectra with some other reheating temperatures after the transition that may be realized in the same model. |
| \it The SNR (upper left panel), the sky localization uncertainty $\Delta \Omega$ (upper middle panel), the polarization uncertainty $\Delta \psi$ (upper right panel), and the uncertainties in the luminosity distance $D_L$ (lower left panel), the time remaining before merger $t_c$ (lower middle panel) and the chirp mass $M_{\rm chirp}$ (lower right panel), calculated for three merging binaries of different BH mass combinations as functions of their redshifts. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to quadratic scalar DM interactions with electrons (left) and photons (right), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza,Hees:2016gop}. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to quadratic scalar DM interactions with electrons (left) and photons (right), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza,Hees:2016gop}. |
| \it Possible experimental scheme. The beams of the two master lasers M1 and M2 are shown as dotted and solid lines, respectively, together with the corresponding reference beams between the satellites, R1 and R2. Two local oscillator lasers LO1 and LO2 (dashed lines) are phase-locked with R2 and R1, respectively. Photodetectors PD1 and PD2 measure the heterodyne beatnote between the reference beams R2 and R1 and the corresponding local lasers LO1 and LO2, respectively, providing feedback for the laser link. Non-polarizing beam splitters are denoted by BS, and tip-tilt mirrors used for controlling the directions of the laser beams are denoted by TTM. For clarity, small offsets between overlapping laser beams have been introduced. Figure taken from~\cite{Graham:2017pmn}. |
| \it Left panel: The sensitivity of AEDGE to the mergers of IMBHs with the contours showing the signal-to-noise ratio (SNR). Right panel: Comparison of the sensitivities of AEDGE, ET and LISA with threshold ${\rm SNR}=8$. {In the lighter regions between the dashed and solid lines the corresponding detector observes only the inspiral phase.} |
| \it Signal-to-noise ratio (SNR) achievable with AEDGE in the parameter plane of the classically scale-invariant extension of the SM with a massive $Z^\prime$ boson. The dashed line is the SNR~$=10$ contour. |
| \it Left panel: The sensitivity of AEDGE to the mergers of IMBHs with the contours showing the signal-to-noise ratio (SNR). Right panel: Comparison of the sensitivities of AEDGE, ET and LISA with threshold ${\rm SNR}=8$. {In the lighter regions between the dashed and solid lines the corresponding detector observes only the inspiral phase.} |
| \it Frequency $f_{\Delta}$ at which features in the cosmic string GW spectrum appear corresponding to events in the early universe occurring at the indicated temperature $T_{\Delta}$. The shading contours indicate $G\mu$ values of the cosmic string network, and the reach of different experiments are indicated by the coloured regions. |
| \it Space-time diagram of the operation of a pair of cold-atom interferometers based on single-photon transitions between the ground state (blue) and the excited state (red dashed). The laser pulses (wavy lines) travelling across the baseline from opposite sides are used to divide, redirect, and recombine the atomic de Broglie waves, yielding interference patterns that are sensitive to the modulation of the light travel time caused by DM or GWs (from~\cite{Graham:2012sy}). For clarity, the sizes of the atom interferometers are shown on an exaggerated scale. |
| \it Left panel: Example of the GW spectrum in a classical scale-invariant extension of the SM with a massive $Z^\prime$ boson, compared with various experimental sensitivities. The dashed line shows the contribution to the spectrum sourced by bubble collisions, the dot-dashed line shows the contribution from sound waves, and the dotted line shows the contribution from turbulence. Right panel: Examples of spectra with some other reheating temperatures after the transition that may be realized in the same model. |
| \it Left panel: The sensitivity of AEDGE to the mergers of IMBHs with the contours showing the signal-to-noise ratio (SNR). Right panel: Comparison of the sensitivities of AEDGE, ET and LISA with threshold ${\rm SNR}=8$. {In the lighter regions between the dashed and solid lines the corresponding detector observes only the inspiral phase.} |
| \it Left panel: The sensitivity of AEDGE to the mergers of IMBHs with the contours showing the signal-to-noise ratio (SNR). Right panel: Comparison of the sensitivities of AEDGE, ET and LISA with threshold ${\rm SNR}=8$. {In the lighter regions between the dashed and solid lines the corresponding detector observes only the inspiral phase.} |
| \it Frequency $f_{\Delta}$ at which features in the cosmic string GW spectrum appear corresponding to events in the early universe occurring at the indicated temperature $T_{\Delta}$. The shading contours indicate $G\mu$ values of the cosmic string network, and the reach of different experiments are indicated by the coloured regions. |
| \it Signal-to-noise ratio (SNR) achievable with AEDGE in the parameter plane of the classically scale-invariant extension of the SM with a massive $Z^\prime$ boson. The dashed line is the SNR~$=10$ contour. |
| \it Comparison of the strain measurements possible with AEDGE and other experiments, showing their sensitivities to BH mergers of differing total masses at various redshifts $z$, indicating also the time remaining before the merger. The solid lines correspond to equal mass binaries and the dashed ones to binaries with very different masses, namely $3000M_\odot$ and $30M_\odot$. Also shown is the possible gravitational gradient noise (GGN) level for a km-scale terrestrial detector, which would need to be mitigated for its potential to be realized. This figure illustrates the potential for synergies between AEDGE and detectors observing other stages of BH infall and merger histories. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to quadratic scalar DM interactions with electrons (left) and photons (right), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza,Hees:2016gop}. |
| \it Left panel: Examples of GW spectra from cosmic strings with differing tensions $G\mu$. The dashed lines show the impact of the variation in the number of SM degrees of freedom. Right panel: Detail of the effect on the GW spectrum for the case $G \mu = 10^{-11}$ of a new particle threshold at various energies $T_\Delta \ge 100$\,MeV with an increase $\Delta g_* = 100$ in the number of relativistic degrees of freedom. |
| \it Left panel: The sensitivity of AEDGE to the mergers of IMBHs with the contours showing the signal-to-noise ratio (SNR). Right panel: Comparison of the sensitivities of AEDGE, ET and LISA with threshold ${\rm SNR}=8$. {In the lighter regions between the dashed and solid lines the corresponding detector observes only the inspiral phase.} |
| \it Left panel: The sensitivity of AEDGE to the mergers of IMBHs with the contours showing the signal-to-noise ratio (SNR). Right panel: Comparison of the sensitivities of AEDGE, ET and LISA with threshold ${\rm SNR}=8$. {In the lighter regions between the dashed and solid lines the corresponding detector observes only the inspiral phase.} |
| \it Possible experimental scheme. The beams of the two master lasers M1 and M2 are shown as dotted and solid lines, respectively, together with the corresponding reference beams between the satellites, R1 and R2. Two local oscillator lasers LO1 and LO2 (dashed lines) are phase-locked with R2 and R1, respectively. Photodetectors PD1 and PD2 measure the heterodyne beatnote between the reference beams R2 and R1 and the corresponding local lasers LO1 and LO2, respectively, providing feedback for the laser link. Non-polarizing beam splitters are denoted by BS, and tip-tilt mirrors used for controlling the directions of the laser beams are denoted by TTM. For clarity, small offsets between overlapping laser beams have been introduced. Figure taken from~\cite{Graham:2017pmn}. |
| \it Left panel: Examples of GW spectra from cosmic strings with differing tensions $G\mu$. The dashed lines show the impact of the variation in the number of SM degrees of freedom. Right panel: Detail of the effect on the GW spectrum for the case $G \mu = 10^{-11}$ of a new particle threshold at various energies $T_\Delta \ge 100$\,MeV with an increase $\Delta g_* = 100$ in the number of relativistic degrees of freedom. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to linear scalar DM interactions with electrons (top), photons (middle) and via the Higgs portal (bottom), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza, Hees:2016gop}. |
| \it Left panel: Example of the GW spectrum in a classical scale-invariant extension of the SM with a massive $Z^\prime$ boson, compared with various experimental sensitivities. The dashed line shows the contribution to the spectrum sourced by bubble collisions, the dot-dashed line shows the contribution from sound waves, and the dotted line shows the contribution from turbulence. Right panel: Examples of spectra with some other reheating temperatures after the transition that may be realized in the same model. |
| \it Left panel: Examples of GW spectra from cosmic strings with differing tensions $G\mu$. The dashed lines show the impact of the variation in the number of SM degrees of freedom. Right panel: Detail of the effect on the GW spectrum for the case $G \mu = 10^{-11}$ of a new particle threshold at various energies $T_\Delta \ge 100$\,MeV with an increase $\Delta g_* = 100$ in the number of relativistic degrees of freedom. |
| \it Possible experimental scheme. The beams of the two master lasers M1 and M2 are shown as dotted and solid lines, respectively, together with the corresponding reference beams between the satellites, R1 and R2. Two local oscillator lasers LO1 and LO2 (dashed lines) are phase-locked with R2 and R1, respectively. Photodetectors PD1 and PD2 measure the heterodyne beatnote between the reference beams R2 and R1 and the corresponding local lasers LO1 and LO2, respectively, providing feedback for the laser link. Non-polarizing beam splitters are denoted by BS, and tip-tilt mirrors used for controlling the directions of the laser beams are denoted by TTM. For clarity, small offsets between overlapping laser beams have been introduced. Figure taken from~\cite{Graham:2017pmn}. |
| \it Signal-to-noise ratio (SNR) achievable with AEDGE in the parameter plane of the classically scale-invariant extension of the SM with a massive $Z^\prime$ boson. The dashed line is the SNR~$=10$ contour. |
| \it Left panel: Example of the GW spectrum in a classical scale-invariant extension of the SM with a massive $Z^\prime$ boson, compared with various experimental sensitivities. The dashed line shows the contribution to the spectrum sourced by bubble collisions, the dot-dashed line shows the contribution from sound waves, and the dotted line shows the contribution from turbulence. Right panel: Examples of spectra with some other reheating temperatures after the transition that may be realized in the same model. |
| \it Left panel: Example of the GW spectrum in a classical scale-invariant extension of the SM with a massive $Z^\prime$ boson, compared with various experimental sensitivities. The dashed line shows the contribution to the spectrum sourced by bubble collisions, the dot-dashed line shows the contribution from sound waves, and the dotted line shows the contribution from turbulence. Right panel: Examples of spectra with some other reheating temperatures after the transition that may be realized in the same model. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to quadratic scalar DM interactions with electrons (left) and photons (right), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza,Hees:2016gop}. |
| \it Space-time diagram of the operation of a pair of cold-atom interferometers based on single-photon transitions between the ground state (blue) and the excited state (red dashed). The laser pulses (wavy lines) travelling across the baseline from opposite sides are used to divide, redirect, and recombine the atomic de Broglie waves, yielding interference patterns that are sensitive to the modulation of the light travel time caused by DM or GWs (from~\cite{Graham:2012sy}). For clarity, the sizes of the atom interferometers are shown on an exaggerated scale. |
| \it Frequency $f_{\Delta}$ at which features in the cosmic string GW spectrum appear corresponding to events in the early universe occurring at the indicated temperature $T_{\Delta}$. The shading contours indicate $G\mu$ values of the cosmic string network, and the reach of different experiments are indicated by the coloured regions. |
| \it The SNR (upper left panel), the sky localization uncertainty $\Delta \Omega$ (upper middle panel), the polarization uncertainty $\Delta \psi$ (upper right panel), and the uncertainties in the luminosity distance $D_L$ (lower left panel), the time remaining before merger $t_c$ (lower middle panel) and the chirp mass $M_{\rm chirp}$ (lower right panel), calculated for three merging binaries of different BH mass combinations as functions of their redshifts. |
| \it The SNR (upper left panel), the sky localization uncertainty $\Delta \Omega$ (upper middle panel), the polarization uncertainty $\Delta \psi$ (upper right panel), and the uncertainties in the luminosity distance $D_L$ (lower left panel), the time remaining before merger $t_c$ (lower middle panel) and the chirp mass $M_{\rm chirp}$ (lower right panel), calculated for three merging binaries of different BH mass combinations as functions of their redshifts. |
| \it Left panel: Examples of GW spectra from cosmic strings with differing tensions $G\mu$. The dashed lines show the impact of the variation in the number of SM degrees of freedom. Right panel: Detail of the effect on the GW spectrum for the case $G \mu = 10^{-11}$ of a new particle threshold at an energies $T_\Delta \ge 100$\,MeV with an increase $\Delta g_* = 100$ in the number of relativistic degrees of freedom |
| \it Left panel: Example of the GW spectrum in a classical scale-invariant extension of the SM with a massive $Z^\prime$ boson, compared with various experimental sensitivities. The dashed line shows the contribution to the spectrum sourced by bubble collisions, the dot-dashed line shows the contribution from sound waves, and the dotted line shows the contribution from turbulence. Right panel: Examples of spectra with some other reheating temperatures after the transition that may be realized in the same model. |
| \it Comparison of the strain measurements possible with AEDGE and other experiments, showing their sensitivities to BH mergers of differing total masses at various redshifts $z$, indicating also the time remaining before the merger. Also shown is the possible gravitational gradient noise (GGN) level for a km-scale terrestrial detector, which would need to be mitigated for its potential to be realized. This figure illustrates the potential for synergies between AEDGE and detectors observing other stages of BH infall and merger histories. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to linear scalar DM interactions with electrons (top), photons (middle) and via the Higgs portal (bottom), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza, Hees:2016gop}. |
| \it Left panel: Examples of GW spectra from cosmic strings with differing tensions $G\mu$. The dashed lines show the impact of the variation in the number of SM degrees of freedom. Right panel: Detail of the effect on the GW spectrum for the case $G \mu = 10^{-11}$ of a new particle threshold at an energies $T_\Delta \ge 100$\,MeV with an increase $\Delta g_* = 100$ in the number of relativistic degrees of freedom |
| \it Space-time diagram of the operation of a pair of cold-atom interferometers based on single-photon transitions between the ground state (blue) and the excited state (red dashed). The laser pulses (wavy lines) travelling across the baseline from opposite sides are used to divide, redirect, and recombine the atomic de Broglie waves, yielding interference patterns that are sensitive to the modulation of the light travel time caused by DM or GWs (from~\cite{Graham:2012sy}). For clarity, the sizes of the atom interferometers are shown on an exaggerated scale. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to linear scalar DM interactions with electrons (top), photons (middle) and via the Higgs portal (bottom), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza, Hees:2016gop}. |
| \it Signal-to-noise ratio (SNR) achievable with AEDGE in the parameter plane of the classically scale-invariant extension of the SM with a massive $Z^\prime$ boson. The dashed line is the SNR~$=10$ contour. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to quadratic scalar DM interactions with electrons (left) and photons (right), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza,Hees:2016gop}. |
| \it Left panel: Example of the GW spectrum in a classical scale-invariant extension of the SM with a massive $Z^\prime$ boson, compared with various experimental sensitivities. The dashed line shows the contribution to the spectrum sourced by bubble collisions, the dot-dashed line shows the contribution from sound waves, and the dotted line shows the contribution from turbulence. Right panel: Examples of spectra with some other reheating temperatures after the transition that may be realized in the same model. |
| \it Left panel: Examples of GW spectra from cosmic strings with differing tensions $G\mu$. The dashed lines show the impact of the variation in the number of SM degrees of freedom. Right panel: Detail of the effect on the GW spectrum for the case $G \mu = 10^{-11}$ of a new particle threshold at an energies $T_\Delta \ge 100$\,MeV with an increase $\Delta g_* = 100$ in the number of relativistic degrees of freedom |
| \it Comparison of the strain measurements possible with AEDGE and other experiments, showing their sensitivities to BH mergers of differing total masses at various redshifts $z$, indicating also the time remaining before the merger. The solid lines correspond to equal mass binaries and the dashed ones to binaries with very different masses, namely $3000M_\odot$ and $30M_\odot$. Also shown is the possible gravitational gradient noise (GGN) level for a km-scale terrestrial detector, which would need to be mitigated for its potential to be realized. This figure illustrates the potential for synergies between AEDGE and detectors observing other stages of BH infall and merger histories. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to linear scalar DM interactions with electrons (top), photons (middle) and via the Higgs portal (bottom), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza, Hees:2016gop}. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to quadratic scalar DM interactions with electrons (left) and photons (right), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza,Hees:2016gop}. |
| \it Left panel: Examples of GW spectra from cosmic strings with differing tensions $G\mu$. The dashed lines show the impact of the variation in the number of SM degrees of freedom. Right panel: Detail of the effect on the GW spectrum for the case $G \mu = 10^{-11}$ of a new particle threshold at an energies $T_\Delta \ge 100$\,MeV with an increase $\Delta g_* = 100$ in the number of relativistic degrees of freedom |
| \it Left panel: Example of the GW spectrum in a classical scale-invariant extension of the SM with a massive $Z^\prime$ boson, compared with various experimental sensitivities. The dashed line shows the contribution to the spectrum sourced by bubble collisions, the dot-dashed line shows the contribution from sound waves, and the dotted line shows the contribution from turbulence. Right panel: Examples of spectra with some other reheating temperatures after the transition that may be realized in the same model. |
| \it Left panel: The sensitivity of AEDGE to the mergers of IMBHs with the contours showing the signal-to-noise ratio (SNR). Right panel: Comparison of the sensitivities of AEDGE, ET and LISA with threshold ${\rm SNR}=8$. {In the lighter regions between the dashed and solid lines the corresponding detector observes only the inspiral phase.} |
| \it Space-time diagram of the operation of a pair of cold-atom interferometers based on single-photon transitions between the ground state (blue) and the excited state (red dashed). The laser pulses (wavy lines) travelling across the baseline from opposite sides are used to divide, redirect, and recombine the atomic de Broglie waves, yielding interference patterns that are sensitive to the modulation of the light travel time caused by DM or GWs (from~\cite{Graham:2012sy}). For clarity, the sizes of the atom interferometers are shown on an exaggerated scale. |
| \it Possible experimental scheme. The beams of the two master lasers M1 and M2 are shown as dotted and solid lines, respectively, together with the corresponding reference beams between the satellites, R1 and R2. Two local oscillator lasers LO1 and LO2 (dashed lines) are phase-locked with R2 and R1, respectively. Photodetectors PD1 and PD2 measure the heterodyne beatnote between the reference beams R2 and R1 and the corresponding local lasers LO1 and LO2, respectively, providing feedback for the laser link. Non-polarizing beam splitters are denoted by BS, and tip-tilt mirrors used for controlling the directions of the laser beams are denoted by TTM. For clarity, small offsets between overlapping laser beams have been introduced. Figure taken from~\cite{Graham:2017pmn}. |
| \it Left panel: The sensitivity of AEDGE to the mergers of IMBHs with the contours showing the signal-to-noise ratio (SNR). Right panel: Comparison of the sensitivities of AEDGE, ET and LISA with threshold ${\rm SNR}=8$. {In the lighter regions between the dashed and solid lines the corresponding detector observes only the inspiral phase.} |
| \it Comparison of the strain measurements possible with AEDGE and other experiments, showing their sensitivities to BH mergers of differing total masses at various redshifts $z$, indicating also the time remaining before the merger. Also shown is the possible gravitational gradient noise (GGN) level for a km-scale terrestrial detector, which would need to be mitigated for its potential to be realized. This figure illustrates the potential for synergies between AEDGE and detectors observing other stages of BH infall and merger histories. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to quadratic scalar DM interactions with electrons (left) and photons (right), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza,Hees:2016gop}. |
| \it Left panel: Example of the GW spectrum in a classical scale-invariant extension of the SM with a massive $Z^\prime$ boson, compared with various experimental sensitivities. The dashed line shows the contribution to the spectrum sourced by bubble collisions, the dot-dashed line shows the contribution from sound waves, and the dotted line shows the contribution from turbulence. Right panel: Examples of spectra with some other reheating temperatures after the transition that may be realized in the same model. |
| \it Possible experimental scheme. The beams of the two master lasers M1 and M2 are shown as dotted and solid lines, respectively, together with the corresponding reference beams between the satellites, R1 and R2. Two local oscillator lasers LO1 and LO2 (dashed lines) are phase-locked with R2 and R1, respectively. Photodetectors PD1 and PD2 measure the heterodyne beatnote between the reference beams R2 and R1 and the corresponding local lasers LO1 and LO2, respectively, providing feedback for the laser link. Non-polarizing beam splitters are denoted by BS, and tip-tilt mirrors used for controlling the directions of the laser beams are denoted by TTM. For clarity, small offsets between overlapping laser beams have been introduced. Figure taken from~\cite{Graham:2017pmn}. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to quadratic scalar DM interactions with electrons (left) and photons (right), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza,Hees:2016gop}. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to quadratic scalar DM interactions with electrons (left) and photons (right), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza,Hees:2016gop}. |
| \it Left panel: The sensitivity of AEDGE to the mergers of IMBHs with the contours showing the signal-to-noise ratio (SNR). Right panel: Comparison of the sensitivities of AEDGE, ET and LISA with threshold ${\rm SNR}=8$. {In the lighter regions between the dashed and solid lines the corresponding detector observes only the inspiral phase.} |
| \it Signal-to-noise ratio (SNR) achievable with AEDGE in the parameter plane of the classically scale-invariant extension of the SM with a massive $Z^\prime$ boson. The dashed line is the SNR~$=10$ contour. |
| \it The sensitivities of AEDGE in broadband (purple lines) and resonant mode (orange lines) to quadratic scalar DM interactions with electrons (left) and photons (right), compared to those of a km-scale terrestrial experiment (green lines). The grey regions show parameter spaces that have been excluded by the MICROSCOPE experiment (blue lines)~\cite{Berge:2017ovy,Hees:2018fpg}, searches for violations of the equivalence principle with torsion balances (red lines)~\cite{Schlamminger:2007ht,Wagner:2012ui}, or by atomic clocks (brown lines)~\cite{VanTilburg:2015oza,Hees:2016gop}. |
| \it Left panel: Examples of GW spectra from cosmic strings with differing tensions $G\mu$. The dashed lines show the impact of the variation in the number of SM degrees of freedom. Right panel: Detail of the effect on the GW spectrum for the case $G \mu = 10^{-11}$ of a new particle threshold at various energies $T_\Delta \ge 100$\,MeV with an increase $\Delta g_* = 100$ in the number of relativistic degrees of freedom. |
| \it Left panel: The sensitivity of AEDGE to the mergers of IMBHs with the contours showing the signal-to-noise ratio (SNR). Right panel: Comparison of the sensitivities of AEDGE, ET and LISA with threshold ${\rm SNR}=8$. {In the lighter regions between the dashed and solid lines the corresponding detector observes only the inspiral phase.} |
| \it Frequency $f_{\Delta}$ at which features in the cosmic string GW spectrum appear corresponding to events in the early universe occurring at the indicated temperature $T_{\Delta}$. The shading contours indicate $G\mu$ values of the cosmic string network, and the reach of different experiments are indicated by the coloured regions. |
| \it Space-time diagram of the operation of a pair of cold-atom interferometers based on single-photon transitions between the ground state (blue) and the excited state (red dashed). The laser pulses (wavy lines) travelling across the baseline from opposite sides are used to divide, redirect, and recombine the atomic de Broglie waves, yielding interference patterns that are sensitive to the modulation of the light travel time caused by DM or GWs (from~\cite{Graham:2012sy}). For clarity, the sizes of the atom interferometers are shown on an exaggerated scale. |